Description
Galaxy's stellar haloes, including their globular cluster populations, are known to build up through the accretion of smaller systems. With Gaia DR3 kinematic data, we uncovered several new small substructures in the local stellar halo, namely the ED-2, 3, 4, 5 and 6; the ED streams. I will present the chemical follow-up of these streams, using targeted high-resolution UVES spectroscopy to unveil their nature. Except for ED-2, all of the streams present a significant spread in [Fe/H] and the chemical signatures of an accreted origin. We homogeneously derive abundances for local Gaia Enceladus stars, to enable direct comparisons. ED-3 and ED-4 exhibit lower [$\alpha$/Fe] compared to GE stars, more similar to the lower mass accreted dwarfs; Sequoia and Helmi Streams. ED-5 and ED-6 are consistent with the GE chemical track and could be high-energy tails of GE that were lost earlier in the accretion process. The abundances of the ED-2 stars are in line with the picture that ED-2 is a disrupted ancient star cluster. I will present chemical abundances for the Gaia BH3 33 M$_\odot$ black hole companion star that is associated with the ED-2 stream and discuss the implications of this system. Our results demonstrate that obtaining high-precision and homogeneous chemical abundances is crucial for disentangling distinct accretion events that have deposited debris in the local halo.
