The core collapse of a massive star in the Milky Way will produce a neutrino burst, intense enough to be detected by existing underground detectors. The AMANDA neutrino telescope located deep in the South Pole ice can detect MeV neutrinos by a collective rate increase in all photo-multipliers on top of dark noise. The main source of light comes from positrons produced in the CC reaction of anti-electron neutrinos on free protons ve + p → e+ + n. This paper describes the first supernova search performed on the full sets of data taken during 1997 and 1998 (215 days of live time) with 302 of the detector's optical modules. No candidate events resulted from this search. The performance of the detector is calculated, yielding a 70% coverage of the galaxy with one background fake per year with 90% efficiency for the detector configuration under study. An upper limit at the 90% c.l. on the rate of stellar collapses in the Milky Way is derived, yielding 4.3 events per year. A trigger algorithm is presented and its performance estimated. Possible improvements of the detector hardware are reviewed.
Bibliographical noteFunding Information:
This research was supported by the US NSF office of Polar Programs and Physics Division, the U. of Wisconsin Alumni Research Foundation, the US DoE, the Swedish Natural Science Research Council, the Swedish Polar Research Secretariat, the Knut and Alice Wallenberg Foundation, Sweden, the German Ministry for Education and Research, the US National Energy Research Scientific Computing Center (supported by the US DoE), UC Irvine AENEAS Supercomputer Facility, and Deutsche Forschungsgemeinschaft (DFG). DFC acknowledges the support of the NSF CAREER program. P. Desiati was supported by the Koerber Foundation (Germany). CPH received support from the EU 4th framework of Training and Mobility of Researchers. St. H. is supported by the DFG (Germany). P. Loaiza was supported by a grant from the Swedish STINT program.
- Dark-noise rate
- Supernova detection