Fig. 1

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6D samples relevant to this work. We selected Gaia Enceladus, Thamnos, and Sequoia, according to Dodd et al. (2023) and defined another sample referred to as the low-energy (LE) sample, shown in magenta. This sample mimics the contamination we expect at low energy for Thamnos, as we can see more clearly in the APOGEE DR17 abundances (bottom row). The top row shows integrals of motion (IoM) space and LAMOST DR7 LRS metallicity distributions normalised and binned each with a relative shift of 0.01 dex to aid in the comparison. The bottom row shows APOGEE DR17 abundances for the different sub-structures, where the Thamnos and Sequoia stars are shown with a black outline.
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