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Did the progenitor of SN 2011dh have a binary companion?
Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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Number of Authors: 9
2015 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 454, no 3, 2580-2585 p.Article in journal (Refereed) Published
Abstract [en]

We present late-time Hubble Space Telescope ultraviolet (UV) and optical observations of the site of SN 2011dh in the galaxy M51, similar to 1164 days post-explosion. At the supernova (SN) location, we observe a point source that is visible at all wavelengths, which is significantly fainter than the spectral energy distribution (SED) of the yellow supergiant progenitor observed prior to explosion. The previously reported photometry of the progenitor is, therefore, completely unaffected by any sources that may persist at the SN location after explosion. In comparison with the previously reported late-time photometric evolution of SN 2011dh, we find that the light curve has plateaued at all wavelengths. The SED of the late-time source is clearly inconsistent with an SED of stellar origin. Although the SED is bright at UV wavelengths, there is no strong evidence that the late-time luminosity originates solely from a stellar source corresponding to the binary companion, although a partial contribution to the observed UV flux from a companion star cannot be ruled out.

Place, publisher, year, edition, pages
2015. Vol. 454, no 3, 2580-2585 p.
Keyword [en]
supernovae: general, supernovae: individual: 2011dh
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-126791DOI: 10.1093/mnras/stv2098ISI: 000368000400026OAI: oai:DiVA.org:su-126791DiVA: diva2:906436
Available from: 2016-02-24 Created: 2016-02-15 Last updated: 2016-02-24Bibliographically approved

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Ergon, Mattias
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The Oskar Klein Centre for Cosmo Particle Physics (OKC)
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