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

Maund, J. R., Arcavi, I., Ergon, M., Eldridge, J. J., Georgy, C., Cenko, S. B., Horesh, A., Izzard, Robert and Stancliffe, R. J. (2015) Did the progenitor of SN 2011dh have a binary companion? Monthly Notices of the Royal Astronomical Society, 454 (3). pp. 2580-2585.

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Abstract

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.

Item Type: Article
Divisions : Faculty of Engineering and Physical Sciences > Physics
Authors :
NameEmailORCID
Maund, J. R.
Arcavi, I.
Ergon, M.
Eldridge, J. J.
Georgy, C.
Cenko, S. B.
Horesh, A.
Izzard, Robertr.izzard@surrey.ac.uk
Stancliffe, R. J.
Date : 13 October 2015
DOI : 10.1093/mnras/stv2098
Depositing User : Karen Garland
Date Deposited : 04 Oct 2018 14:51
Last Modified : 04 Oct 2018 14:51
URI: http://epubs.surrey.ac.uk/id/eprint/849565

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