That supernova could be observed in all details, and it is still being followed. It now emits mainly infrared radiation. It could be followed in all details, close enough in fact that you could determine how much energy is given to the ejected material and that energy is a few times 10⁵¹ erg or, well, between one and two times, and only a small fraction of that, only about 1% of that comes out as light. The main part of that comes out simply as kinetic energy, so you have to observe the Doppler Effect and observe... thereby determine the velocity of the outgoing material, and from that it was possible to determine the energy release. I had some input into that, but the main analysis of that was done by one American and one Japanese astrophysicist, Woosley at University of California, and Nomoto in Tokyo University. They competed, one publishing a paper, then the other publishing a different paper and it is still going on at the present time, and they were able to analyze not only how much energy was released, but also how much nickel-56 was produced. They found out that about 7% of a solar mass of nickel-56 is produced, and that's very interesting because the nickel-56 of course, gives characteristic radiation; it contributes to the optical radiation which was visible; it contributes also gamma rays when the nickel-56 captures electrons and turns into iron-56. And... so it made us... made it possible to understand what really happens in the supernova.