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The Magellanic System's Interactive Formations

Published online by Cambridge University Press:  05 March 2013

M. E. Putman
M. E. Putman*
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Private Bag, Weston Creek PO, ACT 2611, Australia; putman@mso.anu.edu.au
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Abstract

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The interaction between the Galaxy and the Magellanic Clouds has resulted in several high-velocity complexes which are connected to the Clouds. The complexes are known as the Magellanic Bridge, an HI connection between the Large and Small Magellanic Clouds, the Magellanic Stream, a 10° × 100° HI filament which trails the Clouds, and the Leading Arm, a diffuse HI filament which leads the Clouds. The mechanism responsible for these features formation remains under some debate, with the lack of detailed HI observations being one of the limiting factors in resolving the issue. Here I present several large mosaics of HI Parkes All-Sky Survey (HIPASS) data which show the full extent of the three Magellanic complexes at almost twice the resolution of previous observations. These interactive features are connected, but unique in their spatial and velocity distribution. The differences 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 associated with the Magellanic complexes, are also discussed.

Keywords

intergalactic mediumLocal GroupMagellanic Cloudsgalaxies: HI
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 17 , Issue 1 , 2000 , pp. 1 - 5
Copyright
Copyright © Astronomical Society of Australia 2000

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