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Understanding the hydrodynamical processes and conditions at the interfacebetween the Magellanic Stream (MS) and the Galactic halo is critical tounderstanding the MS and by extension, gaseous tails in other interactinggalaxies. These processes operate on relatively small scales and not only helpshape this clumpy stream, but also affect the neutral gas dynamics and transferof mass from the stream to the halo, thus affecting metal enrichment and gasreplenishment of the Galaxy. We describe an observational program to placeconstraints on these processes through high-resolution measurements of HIemission, HI absorption and Halpha emission with unprecedented sensitivity.Methods will include structural analysis, searching for cold gas cores inclumps and analyzing gas kinematics as it transitions to the halo. The lattermethod includes sophisticated spatial integration techniques to deeply probethe neutral gas, which we apply to a new HI map obtained from the Green BankTelescope with the highest sensitivity HI observations of the MS to date. Wedemonstrate that the integration techniques enhance sensitivity even further,thus allowing detection of apparent MS gas components with density approachingthat of the Galactic halo.

The Magellanic Stream to Halo Interface: Processes that shape our nearest gaseous Halo Stream