Comparison of the ﹩\mathrm{log}\,\epsilon ( \mathrm{X}\,) ﹩ abundances of ﹩Z> 30﹩ in HD 221170 with those of CS 22892−052 (blue crosses; Sneden et al. 2003, including upper limits for Ga, Ge, Sn, and U), HD 115444 (green triangles; Westin et al. 2000), BD +17 3248 (red pentagons; Cowan et al. 2002), and the predicted scaled solar r‐process pattern (dotted line; Simmerer et al. 2004). Both the derived and predicted abundances have been normalized to the value derived for ﹩\mathrm{log}\,\epsilon ( \mathrm{Eu}\,) ﹩ in HD 221170. To lessen confusion, upper limits are indicated only for HD 221170. The bottom panel displays the difference defined as ﹩\Delta \mathrm{log}\,\epsilon ( \mathrm{X}\,) \equiv \mathrm{log}\,\epsilon ( \mathrm{X}\,) _{\mathrm{obs}\,}-\mathrm{log}\,\epsilon ( \mathrm{X}\,) _{\mathrm{pred}\,}﹩ for all four r‐process–rich stars with respect to the scaled solar r‐process predictions of Simmerer et al. (2004).