discussed as well as any additional effects or corrections (i.e. hyperfine structure, NLTE, 3D effects, etc.). Hyperfine structure corrections are applied to the elements Sc, V, Mn, Co, Cu, Ba, and La; the isotopic data used to compute the corrections were collected from a variety of sources (Sc, V, Mn, and Co from @b63, additional Mn from @b64, Cu from @Biehl, Ba from @b66, Eu and La from @b67), and the corrections are only found to be significant ($>$0.05 dex) for V and Mn. The abundance errors and standard star comparisons are also discussed in this section.

Abundance Errors {#sec:absens}
----------------

The abundance errors are determined by combining intrinsic random errors in the sample with the errors associated with the stellar parameter uncertainties. The intrinsic errors in the sample are determined by computing the error in the mean (i.e. $\sigma_X$ / $\sqrt{N_\mathrm{X}}$) except in the case where there were fewer than 5 lines of element X, in which case $\sigma_{\mathrm{Fe }}$ / $\sqrt{N_\mathrm{X}}$ is used. The abundance sensitivities due to stellar parameter uncertainties are calculated and summarized for a sample star (NGC 5024-22254) in Table \[table:absens\]. The final errors used with the Galactic comparison are determined by adding the random 