The Large Magellanic Cloud (LMC) is a low-mass irregular galaxy, interacting with the Milky Way (MW) and the Small Magellanic Cloud (SMC). The figure above, from a recent paper by Livingston et al. , shows the HI (neutral hydrogen) distribution of the LMC (as imaged by the ATCA in the 1990s) with annotations showing features of the LMC structure. The LMC is 50 kiloparsecs (160,000 light years) from the Sun and is connected to the SMC by an intercloud region called the Magellanic Bridge (MB). The MB is made up of gas that has been tidally stripped/shared from the SMC and brought towards the south of the LMC. The main HI body of the LMC is made up of an almost circular disc with several HI arms. These HI arms are believed to have formed via interactions between the LMC, SMC, and MW. Throughout the LMC there are super-giant shells (SGSs) that pock the HI structure. In the south-east of the LMC is a region of large HI density called the south-east HI overdensity (SEHO) and a star forming region called 30 Doradus. Between the LMC and the Galactic Plane of the MW is the Leading Arm. The centre-of-mass proper motion of the LMC points eastward: as such the eastern edge is experiencing compression from the movement of the LMC through the halo of the Milky Way.