Cullinane, LaraMackey, DougalDa Costa, GaryKoposov, SergeyBelokurov, VasilyErkal, DenisKoch, AKunder, ANataf, David M2022-10-132022-10-130035-8711http://hdl.handle.net/1885/274523We 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◦ 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 disc model. This includes a large radial velocity dispersion in the LMC disc plane, and an asymmetric line-of-sight velocity distribution indicative of motions vertically out of the disc plane for some stars. The second field reveals 3D kinematics consistent with an equilibrium disc, and yields Vcirc = 87.7 +- 8.0 km s-1 at a radial distance of ∼10.5 kpc from the LMC centre. This leads to an enclosed mass estimate for the LMC at this radius of (1.8 +- 0.3) x 1010 M.Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Based on data acquired at the Anglo-Australian Observatory. SK is partially supported by National Science Foundation (NSF) grants AST-1813881 and AST1909584 and Heising-Simons foundation grant 2018-1030. DMN acknowledges support from the National Aeronautics and Space Administration (NASA) under award number 80NSSC19K0589. AK gratefully acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation) – Project-ID 138713538 – SFB 881 (‘The Milky Way System’), subprojects A03, A05, and A11.application/pdfen-AU© 2020 The authorsstars: kinematics and dynamicsgalaxies: kinematics and dynamicsMagellanic Cloudsgalaxies: stellar contentgalaxies: structure202010.1093/mnras/staa20482021-11-28