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The spectacular detection of gravitational waves (GWs) from GW 150914 and itsreported association with a gamma-ray burst (GRB) offer new insights into theevolution of massive stars. Here it is shown that no single star of any massand credible metallicity is likely to produce the observed GW signal. Starswith helium cores in the mass range 35 to 133 solar masses encounter the pairinstability and either explode or pulse until the core mass is less than 40solar masses, smaller than the combined mass of the observed black holes. Therotation of more massive helium cores is either braked by interaction with aslowly rotating hydrogen envelope, if one is present, or by mass loss, if oneis not. The very short interval between the GW signal and the observed onset ofthe putative GRB in GW 150914 is also too short to have come from a singlestar. A more probable model for making the gravitational radiation is thedelayed merger of two black holes made by 70 and 90 solar mass stars in abinary system. The more massive component was a pulsational-pair instabilitysupernova before making the first black hole.

The Progenitor of GW 150914