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

多达三分之二的银河系晕球状星团（GC）可能是作为矮星系的一部分而被吸积的。GC本身可能在银河势中被破坏，将它们的恒星贡献给晕场人口。我们想阐明（1）矮星系的贡献银河晕使用GC作为示踪剂，（2）量化GC的贡献领域使用独特的化学签名的所谓的第二代恒星和相空间信息从盖亚DR2和DR3。此外，我们将运行大型的，现实的直接N体模型的GC，包括银河系潮汐场，单和双星星的演变，和集群旋转量化的GC晕相互作用。

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.