M.E. Putman, PASA, 17 (1), 1.
Next Section: Introduction
The Magellanic System's Interactive Formations
M.E. Putman 1
1 Research School of Astronomy & Astrophysics, Weston Creek P.0., ACT 2611, Australia
putman@mso.anu.edu.au
Abstract:
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 medium -- Local Group -- Magellanic Clouds -- galaxies: HI
- Introduction
- Magellanic Complexes
- Is it all Magellanic debris?
- Conclusions
- Acknowledgments
- References
© Copyright Astronomical Society of Australia 1997