connected to the same binary companion, this alleviates some of the concern expressed by A02 and Johnson & Bolte (2002) about the high frequency of potential s$+$r stars. However, at least 50% of the very metal-poor CH stars would need to be s$+$r stars if that is the explanation for the elevated Eu/Ba ratios (see Figure 13 in Cohen [et al.]{} (2003)). As Qian & Wasserburg point out, the frequency of AIC events and the parameters necessary to create them are unknown at this time, but the large fraction of very metal-poor CH stars with high Eu implies that the ability to pollute a companion as a AGB star must be tightly correlated with an r-producing AIC event. Another possible problem these authors mention is the still uncertain nucleosynthesis in AIC, which may or may not produce the r-process.

If we hope to understand the origin of neutron-capture elements in CH stars, we need to measure the abundances of as many heavy elements as possible to see if they are consistent with an s$+$r, or s-only or r-only scenario. In this paper, we present results for another CH star. Because of the combination of large abundance enhancements and atmospheric parameters 