[X/H] vs. [Fe/H] for our sample. C from Suárez-Andrés et al. (2017) for ~4400–6800 K warm targets; N from Suárez-Andrés et al. (2016) for stars with T_eff ~ 4500-6500 K; O from Bertran de Lis et al. (2015) for T_eff ~ 5200–6800 K; Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni from Adibekyan et al. (2012c) for targets with T_eff around 4500-6800 K; S from Costa Silva et al. (2020) for 4900-6800 K; Cu, Zn, Y, Zr, Ba, Nd, and Eu from Delgado Mena et al. (2018) for stars with 4500-6800 K; and La from Mishenina et al. (2016) for 4800-6200 K warm stars are overplotted with gray points. The La values were shifted by 0.2 dex. Mean error on [X/H] is shown in the bottom right corner of each panel, while solar values are indicated by dashed lines.