Individual line abundances of Fe I (filled circles) and Fe II (open circles) lines as a function of line strength (top) and excitation energy of the lower level ﹩E_{\mathrm{low}\,}﹩ (bottom) for a TOP star and an RGB star, respectively. While there is no obvious trend of [Fe/H] with ﹩E_{\mathrm{low}\,}﹩, this is not true for all targets and we do not use the excitation equilibrium as an additional effective temperature indicator.