Pairing Gaia data with simulations to trace the dark and stellar mass distribution of the Milky Way

博士学位的目的是利用星系流、附近的矮星系和其他恒星晕子结构来探测银河系的局部结构和全局动力学特性。博士学位的一部分将集中在大麦哲伦星云对当地恒星晕子结构的影响，以及更广泛地研究银河系潜在的不平衡和时间演化。这样的调查将大量利用当前和未来的盖亚数据，以及正在进行的光谱调查（如APOGEE， GALAH， LAMOST以及未来的（WEAVE， DESI））的信息。我们的模型将在银河系形成和演化的数值模拟的帮助下作为基准。

The aim of the PhD is to probe both local structure and global dynamical properties of the Milky Way using streams, nearby dwarf galaxies and other stellar halo sub-structure. A portion of the PhD will focus on the impact that the Large Magellanic Cloud has on local stellar halo sub-structure, and on the disequilibrium and time evolution of the Milky Way potential more broadly. Such an investigation will make significant use of the current and future Gaia data together with the information from ongoing spectroscopic surveys such as APOGEE, GALAH, LAMOST as well as the future ones (WEAVE, DESI). Our models will be benchmarked with the help of numerical simulations of Milky Way formation and evolution.