Modelling the bar/bulge/disc of the Milky Way in the full cosmological context

Using the chemo-dynamical properties of stellar populations in the Milky Way bulge, in combination with ΛCDM simulations of galaxy formation and evolution, to infer its formation history. We find that the Milky Way bulge is indeed compatible with having a pure in-situ origin and we set constraints on the merger history of the Galaxy. See:

https://ui.adsabs.harvard.edu/abs/2019arXiv191106826F/abstract 

Three bar resonant orbits (two of them are corotating and one is an ILR orbit) extracted from a simulated Milky Way-like barred galaxy in the full cosmological context. The orbits are shown in an inertial frame on the left, and in a frame rotating at the same speed as the bar on the right. The simulations are part of the Auriga suite of cosmological zoom-in simulations.

Credit: F. Fragkoudi & the Auriga Project (see https://ui.adsabs.harvard.edu/abs/2019arXiv191106826F/abstract for more details) - feel free to contact me if you would like a high definition version of this animation.

Modelling the Disc of the Milky Way
...and the features seen in phase-space of the disc in Gaia DR2 see:

https://ui.adsabs.harvard.edu/abs/2019MNRAS.tmp.1815F/abstract

This N-body simulation shows the spontaneous formation of a galactic bar and a boxy/peanut bulge in a self-gravitating stellar disc (where the disc is made up of a thin, kinematically cold, a thick kinematically hot and an intermediate disc). In the video on the right the galaxy is rotated so that the bar is always aligned along the x-axis. In the top panel the face-on xy projection is shown and in the bottom panel the edge-on xz projection can be seen. The simulation has 20 million particles distributed in the disc and the dark matter halo. The time at the top is in Gyrs.