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Article: Fourier modeling of the radio torus surrounding SN 1987A

TitleFourier modeling of the radio torus surrounding SN 1987A
Authors
KeywordsCircumstellar Matter
Radio Continuum: Ism
Shock Waves
Supernova Remnants
Supernovae: Individual (Sn 1987A)
Techniques: Interferometric
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2008, v. 684 n. 1, p. 481-497 How to Cite?
AbstractWe present detailed Fourier modeling of the radio remnant of SN 1987A using high-resolution 9 and 18 GHz data taken with the Australia Telescope Compact Array over the period 1992-2008. We develop a parameterized three-dimensional torus model for the expanding radio shell, in which the emission is confined to an inclined equatorial belt; our model also incorporates both a correction for light-travel time effects and an overall east-west gradient in the radio emissivity. By deriving an analytic expression for the two-dimensional Fourier transform of the projected threedimensional brightness distribution, we can fit our spatial model directly to the interferometric visibility data. This provides robust estimates of the radio morphology at each epoch. The best-fit results suggest a constant remnant expansion at 4000 ± 400 km s -1 over the 16 yr period covered by the observations. The model fits also indicate substantial midlatitude emission, extending to ±40° on either side of the equatorial plane. This likely corresponds to the extraplanar structure seen in Hα and Lyα emission from the supernova reverse shock, and broadly supports hydrodynamic models in which the complex circumstellar environment was produced by a progression of interacting winds from the progenitor. Our model quantifies the clear asymmetry seen in the radio images: we find that the eastern half of the radio remnant is consistently ∼40% brighter than the western half at all epochs, which may result from an asymmetry in the ejecta distribution between these two hemispheres. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/180488
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorNg, CYen_US
dc.contributor.authorGaensler, BMen_US
dc.contributor.authorStaveleySmith, Len_US
dc.contributor.authorManchester, RNen_US
dc.contributor.authorKesteven, MJen_US
dc.contributor.authorBall, Len_US
dc.contributor.authorTzioumis, AKen_US
dc.date.accessioned2013-01-28T01:38:46Z-
dc.date.available2013-01-28T01:38:46Z-
dc.date.issued2008en_US
dc.identifier.citationAstrophysical Journal, 2008, v. 684 n. 1, p. 481-497en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/180488-
dc.description.abstractWe present detailed Fourier modeling of the radio remnant of SN 1987A using high-resolution 9 and 18 GHz data taken with the Australia Telescope Compact Array over the period 1992-2008. We develop a parameterized three-dimensional torus model for the expanding radio shell, in which the emission is confined to an inclined equatorial belt; our model also incorporates both a correction for light-travel time effects and an overall east-west gradient in the radio emissivity. By deriving an analytic expression for the two-dimensional Fourier transform of the projected threedimensional brightness distribution, we can fit our spatial model directly to the interferometric visibility data. This provides robust estimates of the radio morphology at each epoch. The best-fit results suggest a constant remnant expansion at 4000 ± 400 km s -1 over the 16 yr period covered by the observations. The model fits also indicate substantial midlatitude emission, extending to ±40° on either side of the equatorial plane. This likely corresponds to the extraplanar structure seen in Hα and Lyα emission from the supernova reverse shock, and broadly supports hydrodynamic models in which the complex circumstellar environment was produced by a progression of interacting winds from the progenitor. Our model quantifies the clear asymmetry seen in the radio images: we find that the eastern half of the radio remnant is consistently ∼40% brighter than the western half at all epochs, which may result from an asymmetry in the ejecta distribution between these two hemispheres. © 2008. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectCircumstellar Matteren_US
dc.subjectRadio Continuum: Ismen_US
dc.subjectShock Wavesen_US
dc.subjectSupernova Remnantsen_US
dc.subjectSupernovae: Individual (Sn 1987A)en_US
dc.subjectTechniques: Interferometricen_US
dc.titleFourier modeling of the radio torus surrounding SN 1987Aen_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1086/590330en_US
dc.identifier.scopuseid_2-s2.0-52049087129en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-52049087129&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume684en_US
dc.identifier.issue1en_US
dc.identifier.spage481en_US
dc.identifier.epage497en_US
dc.identifier.isiWOS:000258730700034-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridGaensler, BM=34769921200en_US
dc.identifier.scopusauthoridStaveleySmith, L=7004532371en_US
dc.identifier.scopusauthoridManchester, RN=7004270810en_US
dc.identifier.scopusauthoridKesteven, MJ=7004146312en_US
dc.identifier.scopusauthoridBall, L=7102282008en_US
dc.identifier.scopusauthoridTzioumis, AK=7003727686en_US
dc.customcontrol.immutablejt 130807-

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