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We use the APOSTLE $\Lambda$CDM cosmological hydrodynamical simulations ofthe Local Group to study the recent accretion of massive satellites into thehalo of Milky Way (MW)-sized galaxies. These systems are selected to be closeanalogues to the Large Magellanic Cloud (LMC), the most massive satellite ofthe MW. The simulations allow us to address, in a cosmological context, theimpact of the Clouds on the MW, including the contribution of Magellanicsatellites to the MW satellite population, and the constraints placed on theGalactic potential by the motion of the LMC. We show that LMC-like satellitesare twice more common around Local Group-like primaries than around isolatedhalos of similar mass; these satellites come from large turnaround radii andare on highly eccentric orbits whose velocities at first pericentre arecomparable with the primary's escape velocity. This implies $V_{\rm esc}^{\rmMW} (50 $ kpc$)\sim 365$ km/s, a strong constraint on Galactic potentialmodels. LMC analogues contribute about 2 satellites with $M_*>10^5\, M_\odot$,having thus only a mild impact on the luminous satellite population of theirhosts. At first pericentre, LMC-associated satellites are close to the LMC inposition and velocity, and are distributed along the LMC's orbital plane. Theirorbital angular momenta roughly align with the LMC's, but, interestingly, theymay appear to "counter-rotate" the MW in some cases. These criteria refineearlier estimates of the LMC association of MW satellites: only the SMC,Hydrus1, Car3, Hor1, Tuc4, Ret2 and Phoenix2 are compatible with all criteria.Carina, Grus2, Hor2 and Fornax are less probable associates given their largeLMC relative velocity.

Magellanic satellites in $\Lambda$CDM cosmological hydrodynamical simulations of the Local Group