Speaker
Description
Since the chemical abundances of stars are the fossil records of the physical conditions in galaxies, they provide the key information for recovering the assembly history of galaxies. In this work, we explore the chemo-chrono-kinematics of accreted and survived dwarf galaxies by analyzing six M31/MW analogues from the HESTIA suite of cosmological hydrodynamics zoom-in simulations of the Local Group. We found that accreted stellar haloes, including individual debris, reveal abundance gradients in the E-Lz space, where the most metal-rich stars have formed in the inner parts of the disrupted systems before the merger and mainly contribute to the central regions of the hosts. Therefore, we suggest that abundance measurements in the inner MW will allow to constrain better the parameters of building blocks of the MW stellar halo. We found that the merger debris are chemically distinct from the survived dwarf galaxies; however, the mergers debris have abundances expected for stars originating from dwarfs that had their star formation activity quenched at early times. Using the data from the APOGEE spectroscopic survey we also explore some other similarities between satellite galaxies and accreted stellar halo of the MW.
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