in this star, we can measure accurate abundances for a number of elements that have been infrequently studied in CH stars. These include Pd, Tb, Ho, Tm and Lu. We have also been able to put interesting limits on the abundance of Th.

Observations
============

CS 31062-050 was selected from a survey of metal-poor star candidates that we have undertaken with the Keck 2 telescope and the intermediate-resolution echelle spectrometer ESI (Sheinis [et al.]{} 2002). The goal of the ESI program is to obtain the abundances of Fe, Ti, Mg, Ca, Ba and in some cases Eu for very metal-poor star candidates and to identify interesting targets for follow-up at higher resolution and bluer wavelengths with Keck 1 and HIRES (Vogt [et al.]{} 1994). CS 31062-050 was identified as a metal-poor star candidate by the UBV photometry of Norris, Ryan & Beers (1999). An ESI spectrum was obtained on 29 August 2000. A single 900s exposure gave a high S/N ($> 100$) spectrum at R$\sim 7000$ from 3900Å to 1$\mu$m. The high carbon abundance of CS 31062-050 was immediately evident from the strength of the G-band. The ESI spectrum also revealed strong and lines. We took higher-resolution spectra with HIRES 