Did the progenitor of SN 2011dh have a binary companion?

J. R. Maund*, I. Arcavi, M. Ergon, J. J. Eldridge, C. Georgy, S. B. Cenko, A. Horesh, R. G. Izzard, R. J. Stancliffe

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

36 Scopus citations


We present late-time Hubble Space Telescope ultraviolet (UV) and optical observations of the site of SN 2011dh in the galaxy M51, ~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.

Original languageAmerican English
Pages (from-to)2580-2585
Number of pages6
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
StatePublished - 11 Dec 2015
Externally publishedYes

Bibliographical note

Publisher Copyright:
© 2015 The Author.


  • Supernovae: general
  • Supernovae: individual: 2011dh


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