The Structure of the Magellanic Stream

Details The Structure of the Magellanic Stream The Structure of the Magellanic Stream

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006atnf.prop..330s&link_type=abstract

ATNF proposal C1197, Semester: April, 2006

Physics

Mag Clouds, Atca

Scientific paper

The HI structure of the Magellanic Stream has proved useful in studying the gravitational and ram-pressure interaction of the Magellanic Clouds with the Galactic Halo, and for investigating the orbital history of the SMC. Previous Parkes observations reveal several tantalising features such as a residual helicity and a transverse velocity gradient which might reflect the binary motion of the SMC and LMC. Also instabilities in the fluid flow from the SMC into the Stream are seen, which might represent interaction with the hot halo gas. Initial analysis of the previously observed pilot region at the head of the Stream have been very encouraging, revealing detail down to 7 arcmin and fully image structures with spatial scales in the range of 0.1-2 kpc. We therefore propose to observe a further 250 deg2 region in the centre of the Stream to build upon the successful pilot observations of the Interface Region and head of the Stream.

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