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Conference Paper: Spectropolarimetry of supernova remnant G296.5 + 10.0

TitleSpectropolarimetry of supernova remnant G296.5 + 10.0
Authors
KeywordsPolarization
Magnetic fields
ISM: supernova remnants
ISM: radio continuum
X-rays: ISM
Issue Date2008
PublisherCambridge University Press.
Citation
International Astronomical Union Symposium S259. In Cosmic Magnetic Fields: From Planets, to Stars and Galaxies-Proceedings of the International Astronomical Union Symposia and Colloquia, 2008, v. 4, p. 141-144 How to Cite?
AbstractRadio continuum emission from the supernova remnant G296.5 + 10.0 was observed using the Australia Telescope Compact Array. Using a 104 MHz bandwidth split into 13 × 8 MHz spectral channels, it was possible to produce a pixel-by-pixel image of Rotation Measure (RM) across the entire remnant. A lack of correlation between RM and X-ray surface brightness reveals that the RMs originate from outside the remnant. Using this information, we will characterise the smooth component of the magnetic field within the supernova remnant and attempt to probe the magneto-ionic structure and turbulent scale sizes in the ISM and galactic halo along the line-of-sight.
Persistent Identifierhttp://hdl.handle.net/10722/185543
ISBN
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorHarvey-Smith, L-
dc.contributor.authorGaensler, BM-
dc.contributor.authorNg, CY-
dc.contributor.authorGreen, AJ-
dc.date.accessioned2013-08-20T07:02:28Z-
dc.date.available2013-08-20T07:02:28Z-
dc.date.issued2008-
dc.identifier.citationInternational Astronomical Union Symposium S259. In Cosmic Magnetic Fields: From Planets, to Stars and Galaxies-Proceedings of the International Astronomical Union Symposia and Colloquia, 2008, v. 4, p. 141-144-
dc.identifier.isbn978-0521889902-
dc.identifier.urihttp://hdl.handle.net/10722/185543-
dc.description.abstractRadio continuum emission from the supernova remnant G296.5 + 10.0 was observed using the Australia Telescope Compact Array. Using a 104 MHz bandwidth split into 13 × 8 MHz spectral channels, it was possible to produce a pixel-by-pixel image of Rotation Measure (RM) across the entire remnant. A lack of correlation between RM and X-ray surface brightness reveals that the RMs originate from outside the remnant. Using this information, we will characterise the smooth component of the magnetic field within the supernova remnant and attempt to probe the magneto-ionic structure and turbulent scale sizes in the ISM and galactic halo along the line-of-sight.-
dc.languageeng-
dc.publisherCambridge University Press.-
dc.relation.ispartofCosmic Magnetic Fields: From Planets, to Stars and Galaxies-Proceedings of the International Astronomical Union Symposia and Colloquia-
dc.rightsCosmic Magnetic Fields: From Planets, to Stars and Galaxies-Proceedings of the International Astronomical Union Symposia and Colloquia. Copyright © Cambridge University Press .-
dc.subjectPolarization-
dc.subjectMagnetic fields-
dc.subjectISM: supernova remnants-
dc.subjectISM: radio continuum-
dc.subjectX-rays: ISM-
dc.titleSpectropolarimetry of supernova remnant G296.5 + 10.0en_US
dc.typeConference_Paperen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hk-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1017/S1743921309030373-
dc.identifier.volume4-
dc.identifier.spage141-
dc.identifier.epage144-
dc.identifier.isiWOS:000266769600037-
dc.publisher.placeUK-
dc.description.otherInternational Astronomical Union Symposium S259. In Cosmic Magnetic Fields: From Planets, to Stars and Galaxies-Proceedings of the International Astronomical Union Symposia and Colloquia, 2008, v. 4, p. 141-144-

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