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dc.contributor.authorHurley-Walker, Natasha
dc.contributor.authorDavies, M.
dc.contributor.authorFranzen, Thomas
dc.contributor.authorGrainge, K.
dc.contributor.authorGreen, D.
dc.contributor.authorHobson, M.
dc.contributor.authorLasenby, A.
dc.contributor.authorPooley, G.
dc.contributor.authorRodriguez-Gonzalvez, C.
dc.contributor.authorSaunders, R.
dc.contributor.authorScaife, A.
dc.contributor.authorScott, P.
dc.contributor.authorShimwell, T.
dc.contributor.authorTitterington, D.
dc.contributor.authorWaldram, E.
dc.contributor.authorZwart, J.
dc.identifier.citationHurley-Walker, N. and Davies, M. and Franzen, T. and Franzen, T. and Grainge, K. and Green, D. and Hobson, M. et al. 2009. G64.5+0.9: a new shell supernova remnant with unusual central emission. Monthly Notices of the Royal Astronomical Society. 398: pp. 249-254.

We present observations between 1.4 and 18 GHz con?rming that G64.5+0.9 is a new Galacticshell supernova remnant, using the Very Large Array and the Arcminute Microkelvin Imager.The remnant is a shell 8 arcmin in diameter with a spectral index of a = 0.47 ± 0.03 (witha de?ned such that ?ux density S varies with frequency ? as S ? ?-a). There is also emissionnear the centre of the shell,1 arcmin in extent, with a spectral index of a =0.81±0.02. Wedo not ?nd any evidence for spectral breaks for either source within our frequency range. Thenature of the central object is unclear and requires further investigation, but we argue that itis most unlikely to be extragalactic. It is dif?cult to avoid the conclusion that it is associatedwith the shell, although its spectrum is very unlike that of known pulsar wind nebulae.

dc.publisherOxford University Press
dc.subjectradiation mechanisms: non-thermal
dc.subjectsupernova remnants
dc.subjectradio continuum: ISM
dc.titleG64.5+0.9: a new shell supernova remnant with unusual central emission
dc.typeJournal Article
dcterms.source.titleMonthly Notices of the Royal Astronomical Society
curtin.accessStatusOpen access via publisher

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