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The many streams of the Magellanic Stream

Published online by Cambridge University Press:  01 July 2008

Snežana Stanimirović ,
Samantha Hoffman ,
Carl Heiles ,
Kevin A. Douglas ,
Mary Putman  and
Joshua E. G. Peek
Snežana Stanimirović
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706, USA email: sstanimi@astro.wisc.edu
Samantha Hoffman
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706, USA email: sstanimi@astro.wisc.edu
Carl Heiles
Affiliation:
Department of Astronomy, UC Berkeley, 601 Campbell Hall, Berkeley, CA 94720, USA
Kevin A. Douglas
Affiliation:
Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
Mary Putman
Affiliation:
University of Michigan, Department of Astronomy, 500 Church St., Ann Arbor, MI 48109, USA
Joshua E. G. Peek
Affiliation:
Department of Astronomy, UC Berkeley, 601 Campbell Hall, Berkeley, CA 94720, USA
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Abstract

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As a part of the ongoing H i survey by the consortium for Galactic studies with the Arecibo L-band Feed Array (GALFA-HI), we have recently imaged the tip of the MS and found several long filamentary structures. This demonstrates that the northern portion of the MS, which has been interacting with the Galactic halo for a long time, is more extended than previously thought and in the form of highly organized H i structures. The observed filaments, and especially the kinematic dichotomy of H i clouds observed for the first time, agree with predictions by the Connors, Kawata & Gibson (2006) tidal model. However, specific time-stamps in the history of the Magellanic System are required to explain these phenomena. The 20-degree long filaments are accompanied by a large population of small H i clouds. We investigate the observed properties of these clouds and explore various instabilities that affect a warm tail of gas trailing through the Galactic halo. Interestingly, if the observed H i structure is mainly due to thermal instability, then the tip of the MS is at a distance of ~70 kpc.

Keywords

ISM: structureGalaxy: halogalaxies: interactionsintergalactic mediumgalaxies: ISMMagellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S256: The Magellanic System: Stars, Gas, and Galaxies , July 2008 , pp. 129 - 134
Copyright
Copyright © International Astronomical Union 2009

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