Uncovering the Galactic stellar halo build-up through chemo-dynamics of globular clusters (A08)

多达三分之二的银晕球状星团(GC)可能是作为矮小星系的一部分而聚集在一起的。GCS本身可能会在银河系势能中被破坏，从而将它们的恒星贡献给晕场人口。我们想要阐明(1)使用GCs作为示踪剂的矮星系对银晕的贡献，以及(2)利用所谓的第二代恒星的独特化学特征和来自Gaia DR2和DR3的相空间信息来量化GC对银晕的贡献。此外，我们将运行大型的、现实的GC直接N体模型，包括银河系潮汐场、单星和双星演化以及星团旋转，以量化GC-Halo相互作用。

Up to two thirds of the Galactic halo globular clusters (GCs) may have been accreted as part of dwarf galaxies. GCs themselves may get disrupted in the Galactic potential, contributing their stars to the halo field population. We want to elucidate (1) the dwarf galaxy contribution to the Galactic halo using GCs as tracers, and (2) quantify the GC contribution to the field using the unique chemical signature of so-called second-generation stars and phase space information from Gaia DR2 and DR3. Moreover, we will run large, realistic direct N-body models of GCs including Galactic tidal fields, single and binary star evolution, and cluster rotation to quantify the GC-halo interaction.