Detection of a γ-ray burst of very long duration and very high energy
Cline, T.; Hurley, K.; Fishman, G. J.; Kouveliotou, C.; Sommer, M.; Boer, M.; Niel, M.; Thompson, D. J.; Mukherjee, R.; Sreekumar, P.; Meegan, C.; Kanbach, G.; Dingus, B. L.; Lin, Y.; Band, D.; Ford, L.; Bertsch, D.; Fichtel, C.; Hartman, R.; Hunter, S.; Mayer-Hasselwander, H.; von Montigny, C.; Nolan, P.; Michelson, P.; Kniffen, D.; Mattox, J.; Schneid, E.
Abstract
ALTHOUGH γ-ray bursts (GRBs) have been known for more than 20 years, their origin remains mysterious1. Suggestions have ranged from nearby colliding comets2 to merging neutron stars at cosmological distances3. The lack of any counterpart at wavelengths other than X-rays and γ-rays has posed a major problem in identifying the source of GRBs4. Although in principle the distribution of energies among the burst photons, as well as their light curves, may be used to constrain the potential sources, this has proved difficult in practice5. Here we present the observation of a particularly energetic burst with a duration of 90 minutes, which includes the detection of an 18-GeV photon. For comparison, typical GRBs emit photons in the energy range between a few keV and a few tens of MeV, and last a few tens of seconds6,7. The extended nature of this burst holds out the hope that there will be opportunities for telescopes operating at other wavelengths to detect a GRB source while it is still active, thus providing further constraints on the source's identity and properties.