can help identify members in the tidal feature. It is also worth nothing that NGC5466 has a retrograde orbit, suggestive of an extragalactic origin [@b56; @b32]. NGC5024 may be linked by a stellar bridge to NGC5053 [@b53; @b50], although no bridge was seen by [@b54], and detailed chemical abundances of stars in these two can be used to study if their formation was coeval.

Detailed chemical abundances have been determined for a few stars in these clusters; one star in NGC5024 and two stars in NGC5466 by [@b57] (at lower resolution and S/N than discussed in this paper, see Section \[sec:obs\]), and one anomalous cepheid in NGC5466 by [@b30]. Iron abundances for several stars in NGC5024 have also been estimated from photometry by [@b10]. All of these analyses confirm the metallicities of \[Fe/H\] $\sim -2$ dex [@b7]. Carbon abundances have been derived from CN and CH band strengths for over a dozen stars in both NGC 5024 and NGC5466 from [@b46] and [@b21], respectively. In both clusters, large variations in the \[C/Fe\] ratios are found, typical of stars that have undergone deep mixing on the red giant branch.

In this paper, we determine the chemical composition of individual stars in 