Speaker
Description
The upcoming GaiaNIR mission will provide unprecedented proper motion measurements for stars across the Local Group, extending Gaia’s capabilities into the near-infrared and enabling the inclusion of stars previously obscured by dust. This will improve orbit determinations for the Milky Way’s satellite dwarf galaxies, and neighboring galaxies such as M31 and M33. In this context, cosmological simulations of the Local Group offer a critical framework to interpret the new data, connect observed dynamics to galaxy formation histories, and place individual systems in a broader cosmic environment.
I will discuss the requirements and characteristics of simulations that are particularly well suited to complement GaiaNIR. High-resolution simulations capable of resolving satellite dwarf galaxies and their stellar halos can link observed dynamics to infall times, tidal interactions, and assembly histories. Such simulations can help constrain the mass distribution of the Milky Way and the total Local Group, and predict the fate of major systems such as M31, M33, and the LMC.
GaiaNIR’s near-infrared sensitivity will improve star member selection in dwarf galaxies, better distinguishing them from Milky Way foreground, and potentially revealing new low-mass satellites or stellar overdensities near the Galactic disc. I will explore how simulations can guide the interpretation of these discoveries, including predictions for previously undetected satellites and signatures of tidal stripping.
By combining the enhanced observational capabilities of GaiaNIR with tailored cosmological simulations, we can unlock a richer understanding of the Local Group beyond the Milky Way, placing its formation and evolution within a cosmological context.
