  We present an overview of, and first science results from, the Magellanic
Edges Survey (MagES), an ongoing spectroscopic survey mapping the kinematics of
red clump and red giant branch stars in the highly substructured periphery of
the Magellanic Clouds. In conjunction with Gaia astrometry, MagES yields a
sample of ~7000 stars with individual 3D velocities that probes larger
galactocentric radii than most previous studies. We outline our target
selection, observation strategy, data reduction and analysis procedures, and
present results for two fields in the northern outskirts ($>10^{\circ}$ on-sky
from the centre) of the Large Magellanic Cloud (LMC). One field, located in the
vicinity of an arm-like overdensity, displays apparent signatures of
perturbation away from an equilibrium disk model. This includes a large radial
velocity dispersion in the LMC disk plane, and an asymmetric line-of-sight
velocity distribution indicative of motions vertically out of the disk plane
for some stars. The second field reveals 3D kinematics consistent with an
equilibrium disk, and yields $V_{\text{circ}}=87.7\pm8.0$km s$^{-1}$ at a
radial distance of ~10.5kpc from the LMC centre. This leads to an enclosed mass
estimate for the LMC at this radius of
$(1.8\pm0.3)\times10^{10}\text{M}_{\odot}$.
