Dependence of iron abundance in BD+46°442 on EWs and the lower excitation potentials of individual lines for our preferred model atmosphere T_eff/log g/V_tur = 6250/1.5/4.0. T_eff was constrained from fits to hydrogen lines, V_tur from the requirement of no trend of individual Fe II abundances with EWs, and log g from the agreement between the iron abundance inferred from Fe II and weak Fe I lines (strong Fe I lines being more affected by non-LTE). The lower panel is less conclusive owing to the non-uniform coverage of the excitation potentials by the Fe II lines. The dashed line indicates the iron abundance of the Sun.