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Recent studies have reported the detection of the galactic stellar halo wakeand dipole triggered by the Large Magellanic Cloud (LMC), mirroring thecorresponding response from dark matter (DM). These studies open up thepossibility of adding constraints on the global mass distribution of the MilkyWay (MW), and even on the nature of DM itself, with current and upcomingstellar surveys reigniting the discussion on response modes in dynamicalfriction. However, the simulation of such features remains computationallychallenging. We used a collisionless Boltzmann equation (CBE)+Poisson solverbased on an existing method from the literature. We investigated the densityand velocity response modes in simulations of Galactic-type DM halos accretingLMC-sized satellites, including the dependence on the halo density profile. Wesuccessfully captured both the local wake and the global over- and underdensityinduced in the host halo. We also captured the velocity response. In line withprevious studies, we find that the code can reproduce the core formation in thecuspy profile and the satellite core stalling. The angular power spectrum (APS)response is shown to be sensitive to each density profile. The cored Plummerdensity profile seems the most responsive, displaying a richness of modes. Atthe end of the simulation, the central halo acquires cylindrical rotation. TheCBE description makes it tenable to capture the response modes with a betterhandling of noise in comparison to traditional N-body simulations. Hence, givena certain noise level, BPM has a lower computational cost than N-bodysimulations, making it feasible to explore large parameter sets. We anticipatethat stellar spheroids in the MW or external galaxies could show centralcylindrical rotation if they underwent a massive accretion event. The code canbe adjusted to include a variety of DM physics.

Boltzmann-Poisson-like approach to simulating the galactic halo response to satellite accretion Dependence on the halo density profile