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tokens: enhanced, so Tri II does not follow the strange K–Mg anticorrelation in NGC 2419. Note that the halo sample here is different than in Figures 2 and 4 because our usual halo compilation does not have K abundances (Frebel 2010 ). Adapted from Venn et al. ( 2017 ). 4.4. Iron-peak Elements: Cr, Mn, Co, Ni, Zn The Fe-peak abundances were determined with equivalent widths, except for Mn, which is synthesized owing to hyperfine structure (Kurucz Bell 1995 ). In Gru I we can constrain Cr, Mn, Co, and Ni, finding that both stars have essentially identical abundances of these elements. Though the Cr and Mn abundances are similar to those in metal-poor stars in other UFDs or in the Milky Way halo, the Co and Ni abundances are somewhat higher. However, this difference is not very significant, especially for Co, which is derived from only a few bluer lines. One Zn line is marginally detected in GruI-032 with an abundance consistent with the halo trend, though with large uncertainty. In Tri II, we can detect Cr and Ni in TriII-40 and provide upper limits in TriII-46. Mn, Co, and Zn are unconstrained, as they only have strong lines blueward of 5000 Å. The upper limits for Cr and Ni in TriII-46 are uninteresting. For TriII-40, we detect a normal [Cr/Fe] ratio, but Ni appears significantly enhanced ([Ni/Fe] = 0.57 ± 0.16), in agreement with Kirby et al. ( 2017 ) and Venn et al. ( 2017 ). 4.5. Neutron-capture Elements: Sr, Ba, Eu Strontium is detected only in Gru I, as the strong Sr ii lines at 4077 and 4215 Å are out of the range of the Tri II (GRACES) spectra. The abundance of both lines is determined with spectrum synthesis. The Sr abundances in these two stars are very similar, [Sr/Fe] ≈ −2, which is much lower than what is found in most halo stars but similar to most UFDs (Figure 4 ). Barium is measured with four different lines in the Gru I stars including hyperfine structure and isotope splitting (McWilliam 1998 ). We use solar isotope ratios (Sneden et al. 2008 ), but given the low overall abundance, changing this to r - or s -process ratios does not significantly affect our abundances. GruI-032 has a low [Ba/Fe] ≈ −1.6, but GruI-038 has a much higher Ba abundance [Ba/Fe] ≈ −1.0. This is formally only 1.6 σ different, but differential comparison of the line strengths (e.g., the λ 6497 line in Figure 1 ) suggests that the difference is real. We discuss this more in Section 5.1 , but both Ba abundances are low and similar to those in most UFDs. Ba is not detected in either Tri II star, so instead we place 5 σ upper limits. The Ba limit for TriII-40 is [Ba/Fe] −1.25, suggesting a low Ba abundance similar to other UFDs. Kirby et al. ( 2017 ) determined [Sr/Fe] = −1.5 and [Ba/Fe] = −2.4 from their HIRES spectrum of this star, consistent with our upper limit and showing that TriII-40 clearly has very low neutron-capture element abundances. The Ba limit for TriII-46 is only [Ba/Fe] ≲ −0.2, but this is still at the lower envelope of the halo trend (Figure 4 ).