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tokens: low-Mg accreted population is Si-poor relative to the high-Mg population—but this trend starts to blur at metallicities below −1.5. In Figure 9 , we show the APOGEE-2 Jhelum giant and the GES candidates as well as both in situ and accreted GCs (Horta et al. 2020 ), along with all of the 1495 Jhelum pointing stars (light gray points). As seen in Figure 9 , the APOGEE-2 Jhelum giant star falls into the high-Si and high-Mg region that both accreted and in situ GCs occupy, as well as accreted dwarf satellite stars (e.g., Sculptor and Carina) and Milky Way field stars. Thus, based on currently available abundances, we cannot narrow down the origin of the Jhelum stream based on chemistry alone. Figure 9. The [Si/Fe] vs. [Mg/Fe] distributions for all Jhelum pointing stars (small gray points), the APOGEE-2 Jhelum RGB star (blue triangle), high- e metal-rich stars (cyan circles), high- e metal-rich stars with [Al/Fe] 0 (magenta circles), accreted MW GCs (orange circles) and in situ MW disk GCs (gray circles). The accreted GCs (orange) are associated with the GES merger and the H99 streams (see Horta et al. 2020 for details on the accreted/in situ classifications for the GCs). 5. Summary In this study, we looked in detail at stars in the direction of the Jhelum stellar stream, taken from the APOGEE-2 database. By isolating stars that have the proper-motion signal detected for Jhelum stream stars by Bonaca et al. ( 2019 ) and Shipp et al. ( 2019 ) and then fitting this proper-motion-selected sample to an isochrone for a 12 Gyr population with [Fe/H] = −1.4 and [ α /Fe] = 0.4, we identified one member of the Jhelum stellar stream. This Jhelum star is a bright red giant, near the tip of the RGB for the Jhelum population. By looking at the azimuthal and radial components of motion for stars in the six APOGEE-2 fields targeting the Jhelum stream, we identified a group of metal-rich ([Fe/H] > −1.7), high-eccentricity ( e > 0.8) stars that are likely to be part of the debris from the GES merger. We divided this GES-sample into high-Al and low-Al groups to help distinguish stars likely belonging to merger debris, as stars from accreted populations tend to have low [Al/Fe] values. While the errors for the distances to the Jhelum giants are large, and these propagate into derived quantities like energy and angular momentum, we compare the total energy as a function of angular momentum ( L z ) for the Jhelum giants to the GES giants and find that, while both populations have similar angular momenta (both are prograde), the Jhelum giants tend to have higher total energies than the GES giants. The orbit for the APOGEE-2 Jhelum giant and the APOGEE-2 GES giants were integrated forward for 5 Gyr and compared, and their respective orbits do not seem consistent with stars derived from same population. In particular, the orbits for the GES giants are highly radial and tend to stay more confined to the plane than does Jhelum. Unfortunately, at the low metallicities