repeated until the carbon and oxygen abundances converge (typically two iterations). The oxygen uncertainty is first determined exactly as described above with iron, then it is added in quadrature to the value found from re-deriving the oxygen abundance after fluctuating carbon by its maximum error. Finally, nitrogen is found from CN regions using the final carbon abundance (see section \[sec:carbon\] for the regions). The rest of the elements are then synthesized and their abundances determined. The final abundances are shown in Tables \[table:Ab1\] and \[table:Ab2\].

Abundance Results {#sec:hfs}
=================

In this section, the abundance errors and standard star comparison are first addressed before comparing our results with the Galactic sample. The abundances with respect to [Fe$\;$[Roman[1]{}]{}]{} from both wavelength regions are then compared with the literature in Section \[sec:galcomp\]. The reported abundances are with respect to solar, ([@b20]). Galactic comparison stars are taken from [@b27], [@b28] (metal-poor stars), and [@b44] (thick disk stars) and comparison MW clusters are taken from [@b45]. Additional comparison stars for Cu and Zn are included from [@b29]. These comparison stars were chosen because their abundances were determined from high-resolution, high S/N spectra. For each element the specific spectral lines used to compute the abundances are 