of CM05 agree within the uncertainties of this work (see Table \[table:inputParam\]) and so the Fe comparison should yield consistent results. The derived M13 standard star \[Fe/H\] abundance from this work is $-1.57 \pm 0.05$ whereas that of CM05 is $-1.48 \pm 0.05$ and that of @b12 is $-1.50 \pm 0.05$ (after correcting both for different solar Fe abundances). The derived M3 standard star \[Fe/H\] abundance is $-1.33 \pm 0.05$ whereas that of CM05 is $-1.42 \pm 0.05$ (again correcting for different solar Fe abundances). We consider these results in good agreement (see Section \[sec:CMcomp\] for an abundance comparison of all determined elements).

Abundance Analysis of Infrared Data {#sec:iranal}
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Chemical abundances in the IR are determined via spectrum synthesis, and not EWs. EWs are not practical in the IR due to the presence of molecular lines and blends across the entire spectrum. Synthetic spectra are calculated with MOOG using the model atmospheres described in Section \[modelatmospheres\] and the DR10 line list from Matthew Shetrone (Shetrone et al. in prep).

To find the iron abundance a preliminary selection of the most prominent iron lines ($\sim$20) is chosen over the spectral range 15100-16900 Å. The spectral region around each of these 