3, we plot the abundances of CS 31062-050 as well as [$r_{ss}$]{}, [$s_{ss}$]{}, and [$t_{ss}$]{} scaled to match the abundance of La. We use La rather than the more traditional Ba because of the large uncertainties in measuring the Ba abundance (see Appendix).

![The abundance in CS 31062-050 compared with [$s_{ss}$]{}, [$r_{ss}$]{}, and [$t_{ss}$]{}. In all cases the solar abundances were scaled to match the La abundance of CS 31062-050. No solar abundance pattern is a good match to the data, even in a limited Z range.](f3.eps){width="2.5in"}

It is clear that none of [$t_{ss}$]{}, [$s_{ss}$]{} or [$r_{ss}$]{} is a good match to the data. In several respects, [$s_{ss}$]{} is the closest, particularly for explaining elements like La, Ce, Pr, Nd, Tb, Dy, and Ho. However, while Y and Zr are enhanced relative to the majority of metal-poor stars, they are not as abundant as a simple scaling of [$s_{ss}$]{} implies. Pd is also $\sim$ 1 dex below the solar system lines. Pb, on the other hand is above the solar system lines with \[Pb/Fe\]=2.81 and \[Pb/La\]=0.69. Although this value is not as extreme as CS 22183-015 (Johnson & Bolte 2002a) or the stars in Van Eck [et al.]{}(2001), it is 