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The Large Magellanic Cloud (LMC) will induce a dynamical friction (DF) wakeon infall to the Milky Way (MW). The MW's stellar halo will respond to thegravity of the LMC and the dark matter (DM) wake, forming a stellar counterpartto the DM wake. This provides a novel opportunity to constrain the propertiesof the DM particle. We present a suite of high-resolution, windtunnel-stylesimulations of the LMC's DF wake that compare the structure, kinematics, andstellar tracer response of the DM wake in cold DM (CDM), with and withoutself-gravity, vs. fuzzy DM (FDM) with $m_a = 10^{-23}$ eV. We conclude that theself-gravity of the DM wake cannot be ignored. Its inclusion raises the wake'sdensity by $\sim 10\%$, and holds the wake together over larger distances($\sim$ 50 kpc) than if self-gravity is ignored. The DM wake's mass iscomparable to the LMC's infall mass, meaning the DM wake is a significantperturber to the dynamics of MW halo tracers. An FDM wake is more granular instructure and is $\sim 20\%$ dynamically colder than a CDM wake, but withcomparable density. The granularity of an FDM wake increases the stars'kinematic response at the percent level compared to CDM, providing a possibleavenue of distinguishing a CDM vs. FDM wake. This underscores the need forkinematic measurements of stars in the stellar halo at distances of 70-100 kpc.

Structure, Kinematics, and Observability of the Large Magellanic Cloud's Dynamical Friction Wake in Cold vs. Fuzzy Dark Matter