Orateur
Description
In the context of dark matter (DM) searches, it is crucial to quantify and reduce theoretical uncertainties affecting predictions that depend on the DM velocity distribution, including event rates in direct searches, velocity-dependent annihilation rates, and microlensing event rates for DM compact objects. The well-known Eddington inversion formalism for the self-consistent reconstruction of the DM velocity distribution from a Galactic mass model allows one to go beyond the simplistic Maxwellian approximation or direct fits to cosmological simulations. However, this method and its anisotropic extensions can be ill-defined depending on the DM and baryonic content of the galaxy of interest.
In this presentation, I will first discuss the validity range of the Eddington inversion methods from a theoretical perspective, as well as issues such as the impact of the finite boundary of a galactic system on observables relevant to DM searches. Then, even in their theoretical validity range, these methods must be tested against hydrodynamical cosmological simulations to assess their relevance for complex gravitational systems such as Milky-Way-like galaxies. I will therefore discuss the predictivity of these methods based on zoom simulations. Finally, as an application, I will present novel constraints on p-wave suppressed DM annihilation from positron data, and their associated theoretical uncertainties.
