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Due to the small amount of hydrogen (${\leq 0.1M_{\odot}}$) remaining on thesurface of their progenitors, Type IIb supernovae are sensitive probes of themass loss processes of massive stars towards the ends of their lives, includingthe role of binarity. We report late-time Hubble Space Telescope observationsof SN 2011dh in M51, and a brief period of re-brightening and plateau in thephotometric light curve, from $1.8$ to $6.2$ years after the explosion. Theseobservations exclude the role of circumstellar interaction, however a slowrotating magnetar, a significant quantity of radioactive elements or a lightecho could be responsible for the late-time luminosity observed at $t >1000\mathrm{d}$. If the late-time light curve is powered by the decay ofradioactive elements, SN~2011dh is required to have produced $\sim 2.6 \times10^{-3}\,M_{\odot}$ of $\mathrm{^{44}Ti}$, which is significantly in excess ofthe amount inferred from earlier nebular spectra of SN 2011dh itself ormeasured in the Cas A SN remnant. The evolution of the brightness and thecolour of the late-time light curve also supports the role of a light echooriginating from dust with a preferred geometry of a disk of extent $\sim 1.8$to $\sim 2.7\,\mathrm{pc}$ from the SN, consistent with a wind-blown bubble.Accounting for the long term photometric evolution due to a light echo, theflux contribution from a surviving binary companion at ultraviolet wavelengthscan be isolated and corresponds to a star of $\sim 9 - 10M_{\odot}$.

The origin of the late-time luminosity of supernova 2011dh