4088Å using the atomic parameters from Vanture [et al.]{} (1991). No Tc was detected, which supports our conclusion that this not a self-polluting AGB star, although large Tc enhancements would be required for any lines to be visible. Finally, Aoki [et al.]{} (2003) have found radial velocity variations in this star. We conclude that CS 31062-050 is a CH star.

We selected a number of lines with good [$gf$-values]{}. Whenever possible, we used recent laboratory measurements. Our choices for [$gf$-values]{} for the heavy elements are summarized in the Appendix. Hyperfine splitting (HFS) and isotopic splitting (IS) are important for many lines of the heavy elements, and we included them for all the elements with HFS and IS constants for the relevant levels in the literature. These sources are discussed in the Appendix as well. For elements lighter than Cu, we used the linelists of Johnson (2002).

The large enhancements of neutron-capture elements meant that we could measure many lines of heavy elements, including some not identified in the solar atlas of Moore, Minnaert & Houtgaust (1966) or in previous abundance analyses of metal-poor stars. To find other lines that would be useful for abundance analysis, we created lists of all 