Comparison of the abundances of ﹩37\leq Z< 50﹩ in HD 221170 with those of CS 22892−052, HD 115444, BD +17 3248, and the scaled solar r‐process predictions, with symbols and normalization as described in Fig. 11. Here we also add the results for CS 31082−001 (magenta plus signs; Hill et al. 2002). The three panels display the difference [﹩\Delta \mathrm{log}\,\epsilon ( \mathrm{X}\,) \equiv \mathrm{log}\,\epsilon ( \mathrm{X}\,) _{\mathrm{obs}\,}-\mathrm{log}\,\epsilon ( \mathrm{X}\,) _{\mathrm{pred}\,}=\Delta _{r}﹩] and scatter (σ) for all five r‐process–rich stars with respect to the scaled solar r‐process predictions of Qian (2003), Arlandini* (largely 1999; with modifications described in § 5.2), and Simmerer et al. (2004).