Stars as Laboratories for Fundamental Physics - MPP Theory Group

420 Chapter 11
Table 11.2. Neutrino burst at the IMB detector (Bratton et al. 1988).
The time is relative to the first event at 7:35:41.374 ± 0:00:00.050 UT, 23
Feb. 1987. The energy refers to the detected e ± , not to the primary neutrino.
Event Time Angle Energy
[s] [degree] [MeV]
1 0.000 80 ± 10 38 ± 7
2 0.412 44 ± 15 37 ± 7
3 0.650 56 ± 20 28 ± 6
4 1.141 65 ± 20 39 ± 7
5 1.562 33 ± 15 36 ± 9
6 2.684 52 ± 10 36 ± 6
7 5.010 42 ± 20 19 ± 5
8 5.582 104 ± 20 22 ± 5
Table 11.3. Neutrino burst at the Baksan detector (Alexeyev et al. 1987,
1988). The time is relative to the first event at 7:36:06.571 +02.000
−54.000 UT, 23
Feb. 1987. The energy refers to the detected e ± , not to the primary neutrino.
Event Time Energy
[s] [MeV]
0 a 0.000 17.5 ± 3.5
1 5.247 12.0 ± 2.4
2 5.682 18.0 ± 3.6
3 6.957 23.3 ± 4.7
4 12.934 17.0 ± 3.0
5 14.346 20.1 ± 4.0
a Usually attributed to background.
The energy of the electron (positron) can be reconstructed from
the total amount of Cherenkov or scintillation light emitted. For small
energies it is roughly proportional to the number of photomultipliers hit
in a given event. Because of the reaction threshold and recoil effects,
the energy of the primary neutrino in the ν e p → ne + reaction is about
2 MeV larger than the measured e + energy. For the rare νe collisions,