each GC. Abundances are determined from both optical and infrared spectroscopic data. This larger wavelength coverage allows us to determine the abundances of more spectral lines and more elements (e.g., CN, CO, OH, Si, and Al are ubiquitous in the IR yet rare in the optical). We also compare the accuracy of the abundance results between the two wavelength regions (similar to @b58).

Observations and Data Reduction
===============================

Observing Program {#sec:obs}
-----------------

Five red giant branch (RGB) stars have been selected in the outer regions of two globular clusters, NGC 5024 and NGC 5466, for detailed spectral analyses. The locations of these objects are shown in Fig. \[fig:finderchart\] and their fundamental properties are listed in Table 1. Targets were chosen based on their V magnitudes, and V-I colours from the . Foreground contamination is minimal.

Optical spectra were gathered with the High Resolution Spectrograph (HRS, @b61) on the HET[^3]. The HRS was at resolution R = 30,000 with 2x2 pixel binning using the 2 arcsecond fibre. The HRS splits the incoming beam onto two CCD chips, from which the spectral regions regions 6000 - 7000 Å (red chip) and 4800 - 5900 Å (blue chip) were extracted for this work. 