Program: GN-2022B-Q-107

Recently, various kinematic substructures (e.g., Gaia-Enceladus, Gaia-Sausage, Sequioa, and Thamnos) have been discovered that are relics of the large and small-scale accretion events that contributed to the formation of the Milky Way. However, the chemical composition of the stars in each substructure, which plays an important role in understanding the chemical characteristics of their progenitor system in the Galactic halo has not been extensively investigated. Hereby, we propose to obtain high-resolution (R = 40,000) spectra of some of the stars that belong to each substructure, which we call dynamically associated metal-poor (DAMP) stars. We will determine stellar atmospheric parameters (Teff, logg, and [Fe/H]) and various elemental abundances from the obtained high-quality spectra. Detailed chemical composition combined with dynamical properties of the DAMP stars will provide strong constraints on the overall properties (e.g., orbit, mass, star formation history, etc.) of their progenitor dwarf galaxy, and ultimately we will be able to characterize the dwarf galaxies that have contributed to the buildup of the Milky Way.