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

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

2009-08-28

arxiv.org/abs/0908.4218v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

7 pages, 2 figures. To appear in the Proceedings of the Galaxy Wars: Stellar Populations and Star Formation in Interacting Gal

Scientific paper

Understanding the hydrodynamical processes and conditions at the interface between the Magellanic Stream (MS) and the Galactic halo is critical to understanding the MS and by extension, gaseous tails in other interacting galaxies. These processes operate on relatively small scales and not only help shape this clumpy stream, but also affect the neutral gas dynamics and transfer of mass from the stream to the halo, thus affecting metal enrichment and gas replenishment of the Galaxy. We describe an observational program to place constraints on these processes through high-resolution measurements of HI emission, HI absorption and Halpha emission with unprecedented sensitivity. Methods will include structural analysis, searching for cold gas cores in clumps and analyzing gas kinematics as it transitions to the halo. The latter method includes sophisticated spatial integration techniques to deeply probe the neutral gas, which we apply to a new HI map obtained from the Green Bank Telescope with the highest sensitivity HI observations of the MS to date. We demonstrate that the integration techniques enhance sensitivity even further, thus allowing detection of apparent MS gas components with density approaching that of the Galactic halo.

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