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CK Vulpeculae was observed in outburst in 1670-16721, but no counterpart wasseen until 1982, when a bipolar nebula was found at its location. Historically,CK Vul has been considered to be a nova (Nova Vul 1670), but a similarity to'red transients', which are more luminous than classical nova and thought to bethe result of stellar collisions, has re-opened the question of CK Vul'sstatus. Red transients cool to resemble late M-type stars, surrounded bycircumstellar material rich in molecules and dust. No stellar source has beenseen in CK Vul, though a radio continuum source was identified at the expansioncentre of the nebula. Here we report CK Vul is surrounded by chemically richmolecular gas with peculiar isotopic ratios, as well as dust. The chemicalcomposition cannot be reconciled with a nova or indeed any other knownexplosion. In addition, the mass of the surrounding gas is too high for a nova,though the conversion from observations of CO to a total mass is uncertain. Weconclude that CK Vul is best explained as the remnant of a merger of two stars.

Nuclear ashes and outflow in the eruptive star Nova Vul 1670