Hα emission from the Magellanic Bridge

E. Muller*, Q. A. Parker

*Corresponding author for this work

Research output: Contribution to journalArticle

6 Citations (Scopus)

Abstract

We present here a preliminary report and commentary of recently processed observations of H? 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 H? 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 H? 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 Hi features.

Original languageEnglish
Pages (from-to)69-76
Number of pages8
JournalPublications of the Astronomical Society of Australia
Volume24
Issue number2
DOIs
Publication statusPublished - 2007

Keywords

  • Galaxies: interactions
  • Galaxies: ISM
  • ISM: structure
  • Stars: activity
  • Turbulence

Fingerprint Dive into the research topics of 'Hα emission from the Magellanic Bridge'. Together they form a unique fingerprint.

Cite this