and Fe[ii]{} lines for the five NGC 6752 giants analyzed in Y03. The EWs measured in the Magellan data are in very good agreement with those measured in the VLT data. Therefore, for the five NGC 6752 giants, we adopt the same stellar parameters used in Y03. In Figure \[fig:ew\_comps\], we compare the EWs of Fe[i]{} and Fe[ii]{} lines for the comparison star HD 141531. The EWs measured in the Subaru data are in very good agreement with those measured in the VLT data. For HD 141531, we adopt the stellar parameters used in Y03. For the four M 13 giants, we determined the stellar parameters using spectroscopic criteria. As in Y03 and Y05, the model atmospheres were taken from the @kurucz93 local thermodynamic equilibrium (LTE) stellar atmosphere grid and we used the LTE stellar line analysis program [Moog]{} [@moog]. For the effective temperature ([$T_{\rm eff}$]{}), we forced the Fe[i]{} lines to show no trend between abundance and lower excitation potential, i.e., excitation equilibrium. To set the surface gravity ($\log g$), we forced the abundances from Fe[i]{} and Fe[ii]{} to be equal, i.e., ionization equilibrium. We adjusted the microturbulent velocity ($\xi_t$) until there was no trend between abundance and EW. 