Speaker
Description
Dark sector theories naturally lead to multi-component scenarios for dark matter where a sub-component can dissipate energy through self-interactions, allowing efficient dark cooling within galaxies. In this talk, I'll present the first cosmological hydrodynamical simulations of dwarf galaxies where the majority of dark matter is collisionless Cold Dark Matter (CDM), but a sub-component (~6%) is strongly dissipative minimal Atomic Dark Matter (ADM). The simulations demonstrate that the addition of even a small fraction of dissipative dark matter can significantly impact galactic evolution. ADM gas with roughly Standard-Model-like masses and couplings can cool efficiently and gravitationally collapse. These effects can significantly enhance the central densities of dwarf galaxies and alter their internal kinematics and their orbital properties around Milky Way-mass galaxies. As a result, observations of dwarf galaxies such as with Rubin and Roman will provide stringent constraints on such dissipative dark sector models.
