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The element abundance ratios of four low-mass stars with extremely lowmetallicities indicate that the gas out of which the stars formed was enrichedin each case by at most a few, and potentially only one low-energy, supernova.Such supernovae yield large quantities of light elements such as carbon butvery little iron. The dominance of low-energy supernovae is surprising, becauseit has been expected that the first stars were extremely massive, and that theydisintegrated in pair-instability explosions that would rapidly enrich galaxiesin iron. What has remained unclear is the yield of iron from the firstsupernovae, because hitherto no star is unambiguously interpreted asencapsulating the yield of a single supernova. Here we report the opticalspectrum of SMSS J031300.36- 670839.3, which shows no evidence of iron (with anupper limit of 10^-7.1 times solar abundance). Based on a comparison of itsabundance pattern with those of models, we conclude that the star was seededwith material from a single supernova with an original mass of ~60 Mo (and thatthe supernova left behind a black hole). Taken together with the previouslymentioned low-metallicity stars, we conclude that low-energy supernovae werecommon in the early Universe, and that such supernovae yield light elementenrichment with insignificant iron. Reduced stellar feedback both chemicallyand mechanically from low-energy supernovae would have enabled first-generationstars to form over an extended period. We speculate that such stars may perhapshave had an important role in the epoch of cosmic reionization and the chemicalevolution of early galaxies.

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J 031300.36-670839.3