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dc.contributor.authorSchinzel, F.K.
dc.contributor.authorTaylor, G.B.
dc.contributor.authorStockdale, C.J.
dc.contributor.authorGranot, J.
dc.contributor.authorRamirez-Ruiz, E.
dc.date.accessioned2009-03-02T11:25:41Z
dc.date.available2009-03-02T11:25:41Z
dc.date.issued2009
dc.identifier.citationSchinzel , F K , Taylor , G B , Stockdale , C J , Granot , J & Ramirez-Ruiz , E 2009 , ' SN 2001em: NOT SO FAST ' , The Astrophysical Journal , vol. 691 , no. 2 , pp. 1380-1386 . https://doi.org/10.1088/0004-637X/691/2/1380
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 153796
dc.identifier.otherPURE UUID: 93f2ec52-105e-4b3c-90cd-b6a45840eb44
dc.identifier.otherdspace: 2299/2984
dc.identifier.otherScopus: 78650136157
dc.identifier.urihttp://hdl.handle.net/2299/2984
dc.descriptionOriginal article can be found at: http://www.iop.org/EJ/journal/apj Copyright American Astronomical Society / IOP Publishing. DOI: 10.1088/0004-637X/691/2/1380 [Full text of this article is not available in the UHRA]
dc.description.abstractSN 2001em, originally classified as type Ib/c, is a peculiar supernova. It was observed in the radio about two years after its optical detection, showing a rising radio flux with an optically thin spectral slope; it also displayed a large X-ray luminosity (~1041 erg s–1). Thus, it was suspected to harbor a decelerating (by then, mildly) relativistic jet pointing away from us. About three years after its discovery, the optical spectrum of SN 2001em showed a broad Hα line, and it was therefore, reclassified as type IIn. Here, we constrain its proper motion and expansion velocity by analyzing four epochs of VLBI observations, extending to 5.4 years after the SN. The supernova is still unresolved 5.4 years after the explosion. For the proper motion, we obtain (23,000± 30,000) km s–1, while our 2σ upper limit on the expansion velocity is 6000 km s–1. These limits are somewhat tighter than those derived by Bietenholz & Bartel, and confirm their conclusion that late time emission from SN 2001em, a few years after the explosion, is not driven by a relativistic jet. VLA observations of the radio flux density, at 8.46 GHz, show a decay as t –1.23 ± 0.40 starting ~2.7 years after the SN. Collectively, the observations suggest interaction of the SN ejecta with a very dense circumstellar medium, though the implied opacity constraints still present a challenge.en
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.titleSN 2001em: NOT SO FASTen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/691/2/1380
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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