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Hα Emission from the Magellanic Bridge

Published online by Cambridge University Press:  05 March 2013

E. Muller  and
Q. A. Parker
E. Muller*
Affiliation:
Bolton Fellow, Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping NSW 1710, Australia
Q. A. Parker
Affiliation:
Department of Physics, Macquarie University, Sydney NSW 2109, Australia Anglo-Australian Observatory, Epping NSW 1710, Australia
*
DCorresponding author. Email: [email protected]
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Abstract

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We present here a preliminary report and commentary of recently processed observations of Hα emission towards the Magellanic Bridge. These data have been analysed in an attempt to quantify the extent to which the stellar population is capable of reshaping the local ISM. We find that the Hα emission regions are small, weak and sparsely distributed, consistent with a relatively quiescent and inactive ISM where radiative and collisional ionisation is inefficient and sporadic. This suggests that energetic processes at the small scale (i.e. ∼tens of pc) do not dominate the energy balance within the ISM of the Bridge, which therefore hosts a pristine turbulent structure, otherwise inaccessible within our own Galaxy. We find Hα emission that is well correlated with detected 12CO(1–0) line emission (a proxy for molecular hydrogen), as well as other easily identified ring-like Hı features.

Keywords

TurbulenceISM: structuregalaxies: ISMgalaxies: interactionsstars: activity
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 24 , Issue 2 , 2007 , pp. 69 - 76
Copyright
Copyright © Astronomical Society of Australia 2007

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