Combined with ground-based spectroscopic surveys, Gaia DR2 presents an opportunity to study the chemodynamical evolution of the Milky Way (MW) in unprecedented detail. On the theory side, several approaches have been used to complement Gaia's observations. We present a new set of simulations that evolve every single F, G and K star born in the last 5 Gyr in a realistic MW potential that includes a bar, spiral arms and GMCs. The simulation is the first of its kind to include a subgrid model for star cluster dissolution and simultaneously evolve the whole disk star-by-star, allowing us to study the scales at which phase space structure in the disk could be caused by star clusters forming and dissolving and the scales at which resonances play the dominant role. As an example of the power of combining kinematic and chemical information, we examine co-moving pairs in both the simulations and Gaia and find evidence for a high co-natal fraction in the data at high separations and low velocities. In conclusion, this work directly helps us examine the feasibility of uncovering the assembly history of the Milky Way using Gaia and other spectroscopic surveys via a unique set of models.
University
Harvard University