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dc.contributor.authorGomez, H.L.
dc.contributor.authorDunne, L.
dc.contributor.authorIvison, R.J.
dc.contributor.authorReynoso, E.M.
dc.contributor.authorThompson, M.A.
dc.contributor.authorSibthorpe, B.
dc.contributor.authorEales, S.A.
dc.contributor.authorDelaney, T.M.
dc.contributor.authorMaddox, S.
dc.contributor.authorIsaak, K.
dc.date.accessioned2009-12-22T11:52:41Z
dc.date.available2009-12-22T11:52:41Z
dc.date.issued2009
dc.identifier.citationGomez , H L , Dunne , L , Ivison , R J , Reynoso , E M , Thompson , M A , Sibthorpe , B , Eales , S A , Delaney , T M , Maddox , S & Isaak , K 2009 , ' Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant ' , Monthly Notices of the Royal Astronomical Society , vol. 397 , no. 3 , pp. 1621-1632 . https://doi.org/10.1111/j.1365-2966.2009.15061.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 174194
dc.identifier.otherPURE UUID: 4b86bdfe-6133-4c58-9c1a-0ec16e5aed8c
dc.identifier.otherdspace: 2299/4121
dc.identifier.otherBibtex: urn:bbf0cbe9a3e4ad774f26f1c8cc0eb922
dc.identifier.otherScopus: 68149167935
dc.identifier.otherORCID: /0000-0001-5392-909X/work/30970862
dc.identifier.urihttp://hdl.handle.net/2299/4121
dc.description‘The definitive version is available at www3.interscience.wiley.com '. Copyright Royal Astronomical Society. DOI: 10.1111/j.1365-2966.2009.15061.x
dc.description.abstractWhether or not supernovae contribute significantly to the overall dust budget is a controversial subject. Submillimetre (sub-mm) observations, sensitive to cold dust, have shown an excess at 450 and 850 μm in young remnants Cassiopeia A (Cas A) and Kepler. Some of the sub-mm emission from Cas A has been shown to be contaminated by unrelated material along the line of sight. In this paper, we explore the emission from material towards Kepler using sub-mm continuum imaging and spectroscopic observations of atomic and molecular gas, via H i, 12CO(J= 2–1) and 13CO(J= 2–1). We detect weak CO emission (peak T*A = 0.2–1 K, 1–2 km s−1 full width at half-maximum) from diffuse, optically thin gas at the locations of some of the sub-mm clumps. The contribution to the sub-mm emission from foreground molecular and atomic clouds is negligible. The revised dust mass for Kepler's remnant is 0.1–1.2 M⊙ , about half of the quoted values in the original study by Morgan et al., but still sufficient to explain the origin of dust at high redshifts.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectSupernovae: Kepler , ISM: submillimetre dust , radio lines: ISM , Galaxies: abundances , submillimetre
dc.titleAccounting for the foreground contribution to the dust emission towards Kepler's supernova remnanten
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=68149167935&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2009
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2009.15061.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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