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Article: Hα emission from the Magellanic Bridge

TitleHα emission from the Magellanic Bridge
Authors
KeywordsISM: structure
Galaxies: ISM
Stars: activity
Turbulence
Galaxies: interactions
Issue Date2007
Citation
Publications of the Astronomical Society of Australia, 2007, v. 24, n. 2, p. 69-76 How to Cite?
AbstractWe 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. © Astronomical Society of Australia 2007.
Persistent Identifierhttp://hdl.handle.net/10722/208797
ISSN
2015 Impact Factor: 3.245

 

DC FieldValueLanguage
dc.contributor.authorMüller, Erik-
dc.contributor.authorParker, Quentin A.-
dc.date.accessioned2015-03-23T02:01:44Z-
dc.date.available2015-03-23T02:01:44Z-
dc.date.issued2007-
dc.identifier.citationPublications of the Astronomical Society of Australia, 2007, v. 24, n. 2, p. 69-76-
dc.identifier.issn1323-3580-
dc.identifier.urihttp://hdl.handle.net/10722/208797-
dc.description.abstractWe 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. © Astronomical Society of Australia 2007.-
dc.languageeng-
dc.relation.ispartofPublications of the Astronomical Society of Australia-
dc.subjectISM: structure-
dc.subjectGalaxies: ISM-
dc.subjectStars: activity-
dc.subjectTurbulence-
dc.subjectGalaxies: interactions-
dc.titleHα emission from the Magellanic Bridge-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1071/AS07010-
dc.identifier.scopuseid_2-s2.0-34547530085-
dc.identifier.volume24-
dc.identifier.issue2-
dc.identifier.spage69-
dc.identifier.epage76-
dc.identifier.eissn1448-6083-

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