Fig. 7

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Same figure format as in Fig. 4. This star is one of the four Ba stars that was difficult to classify manually because the abundances in the first s-process peak are higher than predicted by the best-fit models (Group 2 stars in Paper I). We found a final classification for this star with our algorithms. However, [Nb/Fe] is too high to be matched by our AGB final surface abundances.
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