The Magellanic system's interactive formations

The interaction between the Galaxy and the Magellanic Clouds has resulted i n several high-velocity complexes which are connected to the Clouds. The co mplexes are known as the Magellanic Bridge, an HI connection between the La rge and Small Magellanic Clouds, the Magellanic Stream, a 10 degrees x 100 degrees HI filament which trails the Clouds, and the Leading Arm, a diffuse HI filament which leads the Clouds. The mechanism responsible for these fe atures formation remains under some debate, with the lack of detailed KI ob servations being one of the limiting factors in resolving the issue. Here I present several large mosaics of HI Parkes All-Sky Survey (HIPASS) data wh ich show the full extent of the three Magellanic complexes at almost twice the resolution of previous observations. These interactive features are con nected, but unique in their spatial and velocity distribution. The differen ces may shed light on their origin and present environment. Dense clumps of HI along the sightline to the Sculptor Group, which may or may not be asso ciated with the Magellanic complexes, are also discussed.