Dark matter in disequilibrium at galactic scales

Dark matter (DM) constitutes approximately 85% of all matter in the Universe, yet its nature remains elusive---we have not observed it directly. Understanding how DM is distributed on galactic scales is essential to constraining its properties and its role in shaping galaxies. In the field of galactic dynamics, we infer the distribution of DM in the Milky Way (MW) by studying stellar motions. Traditionally, this has been done under the assumption of a static and symmetric gravitational potential for the MW. However, in the Gaia era, it is now clear that the MW is dynamically evolving and asymmetric, rendering these static models inadequate. To solve this, we have developed novel potential modeling frameworks that capture the time-evolving, asymmetric nature of the MW, validated using state-of-the-art zoomed cosmological-baryonic simulations. I will present two key applications of these models, demonstrating how they provide new insights into the distribution and behavior of DM on both local and global scales. These advancements offer a new window into DM’s evolving structure and its role in the formation and evolution of galaxies.