  Understanding the physical mechanism behind the formation of a co-rotating
thin plane of satellite galaxies, like the one observed around the Milky Way
(MW), has been challenging. The perturbations induced by a massive satellite
galaxy, like the Large Magellanic Cloud (LMC) provide valuable insight into
this problem. The LMC induces an apparent co-rotating motion in the outer halo
by displacing the inner regions of the halo with respect to the outer halo.
Using the Latte suite of FIRE-2 cosmological simulations of MW-mass galaxies,
we confirm that the apparent motion of the outer halo induced by the infall of
a massive satellite changes the observed distribution of orbital poles of
outer-halo tracers, including satellites. We quantify the changes in the
distribution of orbital poles using the two-point angular correlation function
and find that all satellites induce changes. However, the most massive
satellites with pericentric passages between 30-100kpc induce the largest
changes. The best LMC-like satellite analog shows the largest change in orbital
pole distribution. The dispersion of orbital poles decreases by 20{\deg} during
the first two pericentric passages. Even when excluding the satellites brought
in with the LMC-like satellite, there is clustering of orbital poles. These
results suggest that in the MW, the recent pericentric passage of the LMC
should have changed the observed distribution of orbital poles of all other
satellites. Therefore, studies of kinematically-coherent planes of satellites
that seek to place the MW in a cosmological context should account for the
existence of a massive satellite like the LMC.
