Magellanic satellites in $\Lambda$CDM cosmological hydrodynamical
  simulations of the Local Group
  We use the APOSTLE $\Lambda$CDM cosmological hydrodynamical simulations of
the Local Group to study the recent accretion of massive satellites into the
halo of Milky Way (MW)-sized galaxies. These systems are selected to be close
analogues to the Large Magellanic Cloud (LMC), the most massive satellite of
the MW. The simulations allow us to address, in a cosmological context, the
impact of the Clouds on the MW, including the contribution of Magellanic
satellites to the MW satellite population, and the constraints placed on the
Galactic potential by the motion of the LMC. We show that LMC-like satellites
are twice more common around Local Group-like primaries than around isolated
halos of similar mass; these satellites come from large turnaround radii and
are on highly eccentric orbits whose velocities at first pericentre are
comparable with the primary's escape velocity. This implies $V_{\rm esc}^{\rm
MW} (50 $ kpc$)\sim 365$ km/s, a strong constraint on Galactic potential
models. LMC analogues contribute about 2 satellites with $M_*>10^5\, M_\odot$,
having thus only a mild impact on the luminous satellite population of their
hosts. At first pericentre, LMC-associated satellites are close to the LMC in
position and velocity, and are distributed along the LMC's orbital plane. Their
orbital angular momenta roughly align with the LMC's, but, interestingly, they
may appear to "counter-rotate" the MW in some cases. These criteria refine
earlier 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 large
LMC relative velocity.
