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- Publisher Website: 10.1071/AS07010
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Article: Hα emission from the Magellanic Bridge
Title | Hα emission from the Magellanic Bridge |
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Authors | |
Keywords | ISM: structure Galaxies: ISM Stars: activity Turbulence Galaxies: interactions |
Issue Date | 2007 |
Citation | Publications of the Astronomical Society of Australia, 2007, v. 24, n. 2, p. 69-76 How to Cite? |
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. © Astronomical Society of Australia 2007. |
Persistent Identifier | http://hdl.handle.net/10722/208797 |
ISSN | 2023 Impact Factor: 4.5 2023 SCImago Journal Rankings: 1.688 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Müller, Erik | - |
dc.contributor.author | Parker, Quentin A. | - |
dc.date.accessioned | 2015-03-23T02:01:44Z | - |
dc.date.available | 2015-03-23T02:01:44Z | - |
dc.date.issued | 2007 | - |
dc.identifier.citation | Publications of the Astronomical Society of Australia, 2007, v. 24, n. 2, p. 69-76 | - |
dc.identifier.issn | 1323-3580 | - |
dc.identifier.uri | http://hdl.handle.net/10722/208797 | - |
dc.description.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. © Astronomical Society of Australia 2007. | - |
dc.language | eng | - |
dc.relation.ispartof | Publications of the Astronomical Society of Australia | - |
dc.subject | ISM: structure | - |
dc.subject | Galaxies: ISM | - |
dc.subject | Stars: activity | - |
dc.subject | Turbulence | - |
dc.subject | Galaxies: interactions | - |
dc.title | Hα emission from the Magellanic Bridge | - |
dc.type | Article | - |
dc.description.nature | link_to_subscribed_fulltext | - |
dc.identifier.doi | 10.1071/AS07010 | - |
dc.identifier.scopus | eid_2-s2.0-34547530085 | - |
dc.identifier.volume | 24 | - |
dc.identifier.issue | 2 | - |
dc.identifier.spage | 69 | - |
dc.identifier.epage | 76 | - |
dc.identifier.eissn | 1448-6083 | - |
dc.identifier.isi | WOS:000248401600004 | - |
dc.identifier.issnl | 1323-3580 | - |