was used. We find a 3$\sigma$ limit of log $\epsilon (Th)=-0.85$ and a 5$\sigma$ limit of log $\epsilon (Th) = -0.70$. Our syntheses for these limits are shown in Figure 2.

![Spectral synthesis of the Th line at 4019Å. The solid squares are the data. At \[Th/Fe\]=0, the Th line is so weak that our synthesis is indistinguishable from a synthesis with no Th.](f2.eps){width="3.0in"}

Results
=======

Our abundances and errors are in Table 2. The solar values are adopted from the meteoritic abundances in Grevesse, Noels, & Sauval (1996). Table 2 also includes a comparison with the A02 abundances. Our lower [T$_{\rm eff}$]{} and gravity mean that we have lower log$\epsilon$ in general for the singly-ionized rare earth species, but the offset from A02 is fairly constant. The abundances of the elements between Mg and Ni are in good agreement with metal-poor field stars that are not C-rich or heavy-element-rich studied with the same linelist by Johnson (2002). The “$\alpha$”-elements (Mg, Ca, and Ti) have supersolar \[X/Fe\] ratios. The iron-peak elements track Fe closely with the exception of Mn, whose depletion relative to iron in metal-poor stars was first noted by McWilliam [et al.]{} (1995). Therefore, any explanation of the 