4.7 Article

SEARCH FOR MUON NEUTRINOS FROM GAMMA-RAY BURSTS WITH THE IceCube NEUTRINO TELESCOPE

Journal

ASTROPHYSICAL JOURNAL
Volume 710, Issue 1, Pages 346-359

Publisher

IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/710/1/346

Keywords

gamma-ray burst: general; methods: data analysis; neutrinos; telescopes

Funding

  1. U.S. National Science Foundation-Office
  2. U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation
  3. U.S. Department of Energy
  4. National Energy Research Scientific Computing Center
  5. Louisiana Optical Network Initiative (LONI)
  6. Swedish Research Council
  7. Swedish Polar Research Secretariat
  8. Knut and Alice Wallenberg Foundation, Sweden
  9. German Ministry for Education and Research (BMBF)
  10. Deutsche Forschungsgemeinschaft (DFG), Germany
  11. FNRS-FWO
  12. Flanders Institute
  13. Belgian Federal Science Policy Office (Belspo)
  14. Netherlands Organisation for Scientific Research (NWO)
  15. Marsden Fund, New Zealand
  16. SNF (Switzerland)
  17. EU
  18. Capes Foundation, Ministry of Education of Brazil
  19. Division Of Physics
  20. Direct For Mathematical & Physical Scien [0855241, 0855291] Funding Source: National Science Foundation

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We present the results of searches for high-energy muon neutrinos from 41 gamma-ray bursts (GRBs) in the northern sky with the IceCube detector in its 22 string configuration active in 2007/2008. The searches cover both the prompt and a possible precursor emission as well as a model-independent, wide time window of -1 hr to + 3 hr around each GRB. In contrast to previous searches with a large GRB population, we do not utilize a standard Waxman-Bahcall GRB flux for the prompt emission but calculate individual neutrino spectra for all 41 GRBs from the burst parameters measured by satellites. For all of the three time windows, the best estimate for the number of signal events is zero. Therefore, we place 90% CL upper limits on the fluence from the prompt phase of 3.7 x 10(-3) erg cm(-2) (72 TeV-6.5 PeV) and on the fluence from the precursor phase of 2.3 x 10(-3) erg cm(-2) (2.2-55 TeV), where the quoted energy ranges contain 90% of the expected signal events in the detector. The 90% CL upper limit for the wide time window is 2.7 x 10(-3) erg cm(-2) (3 TeV-2.8 PeV) assuming an E-2 flux.

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