We are studying the chemical and star formation consequences of the dynamical evolution of Local group galaxies. Our goals are to model them in the light of many observations of the Milky way and dwarf galaxies (Gaia, APOGEE, WEAVE etc) and of M31 (PHAT, PHAST, PAndAs, etc).
Numerical simulations include hydrodynamical solver softwares (e.g., GIZMO), for full modelling of M31 properties as a 2.5 Gyr old merger remnant, of the Magellanic stream and its two inter-twisted ram-pressure filaments from the Clouds, and of dwarf galaxies during their fate after their infall.
Combined Gaia orbital data and chemical studies from spectroscopy with 8 meters telescope suggests that the latter have had still recent star-formation and then late infall.
The team models now the Milky way and its Gaia rotation curve. It will achieve modelling of all kind of objects in the Local group to assess their material content.
