a comparison of EW measurements (this work) compared with those from @b2 [hereafter referred to as CM05]. A mean difference (This Study - Literature) of $-0.819$ mÅ ($\sigma = 5.836$ mÅ) is found in M13-III-18 (from 127 lines) and a difference of $-1.599$ mÅ ($\sigma = 5.967$ mÅ) is found for M3-C41303-2217 (from 115 lines). This agreement is reasonable and these measurement methods are applied to the new targets in NGC 5024 and NGC 5466.

Model Atmosphere and Abundance Analysis of Optical Data {#modelatmospheres}
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The optical abundances are computed by using the radiative transfer code MOOG (@b8), which uses stellar model atmospheres and atomic data to synthesize spectra. The new MARCS spherical models have been adapted (@b3 [@b79], also see @b80) assuming \[$\alpha$/Fe\] enhancement since the science targets and standard stars are relatively metal-poor (\[Fe/H\] $<$ -1 dex). This combination of spherical model atmospheres and MOOG’s plane parallel radiative transfer is appropriate for analyzing red giants (e.g. see @b76 and additional tests by @b77).

Photometric Stellar parameters {#sec:stellarparams}
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The stellar parameter $\mathrm{T}_{\mathrm{eff}}$ is computed using the infrared flux method (IRFM, described by @b6), which requires precision photometry, reddening, distance modulus, metallicity, and stellar mass. Using this $\mathrm{T}_{\mathrm{eff}}$ and 