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The core-collapse supernova of a massive star rapidly brightens when a shock,produced following the collapse of its core, reaches the stellar surface. Asthe shock-heated star subsequently expands and cools, its early-time lightcurve should have a simple dependence on the progenitor's size and thereforefinal evolutionary state. Measurements of the progenitor's radius from earlylight curves exist for only a small sample of nearby supernovae, and almost alllack constraining ultraviolet observations within a day of explosion. Theseveral-day time delays and magnifying ability of galaxy-scale gravitationallenses, however, should provide a powerful tool for measuring the early lightcurves of distant supernovae, and thereby studying massive stellar populationsat high redshift. Here we analyse individual rest-frameultraviolet-through-optical exposures taken with the Hubble Space Telescopethat simultaneously capture, in three separate gravitationally lensed images,the early phases of a supernova at redshift $z \approx 3$ beginning within$5.8\pm 3.1$ hr of explosion. The supernova, seen at a lookback time of$\sim11.5$ billion years, is strongly lensed by an early-type galaxy in theAbell 370 cluster. We constrain the pre-explosion radius to be$533^{+154}_{-119}$ solar radii, consistent with a red supergiant. Highlyconfined and massive circumstellar material at the same radius can alsoreproduce the light curve, but is unlikely since no similar low-redshiftexamples are known.

Shock cooling of a red-supergiant supernova at redshift 3 in lensed images