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Title:
Detection of Gamma Rays of up to 50 TeV from the Crab Nebula
Authors:
Tanimori, T.; Sakurazawa, K.; Dazeley, S. A.; Edwards, P. G.; Hara, T.; Hayami, Y.; Kamei, S.; Kifune, T.; Konishi, T.; Matsubara, Y.; Matsuoka, T.; Mizumoto, Y.; Masaike, A.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Oda, S.; Ogio, S.; Osaki, T.; Patterson, J. R.; Roberts, M. D.; Rowell, G. P.; Suzuki, A.; Suzuki, R.; Sako, T.; Tamura, T.; Thornton, G. J.; Susukita, R.; Yanagita, S.; Yoshida, T.; Yoshikoshi, T.
Publication:
Astrophysical Journal Letters v.492, p.L33 (ApJL Homepage)
Publication Date:
01/1998
Origin:
APJ
ApJ Keywords:
GAMMA RAYS: OBSERVATIONS, ISM: INDIVIDUAL NAME: CRAB NEBULA
DOI:
10.1086/311077
Bibliographic Code:
1998ApJ...492L..33T

Abstract

Gamma rays with energies greater than 7 TeV from the Crab pulsar/Crab Nebula have been observed at large zenith angles, with the imaging atmospheric technique from Woomera, South Australia. CANGAROO data taken in 1992, 1993, and 1995 indicate that the energy spectrum extends up to at least 50 TeV, without a change of the index of the power-law spectrum. The observed differential spectrum is (2.01+/-0.36)x10^{-13}(E/7w {TeV})^{-2.53+/-0.18}{TeV}^{-1}{cm}^{-2}{s}^{-1} between 7 and 50 TeV. There is no apparent cutoff. The spectrum for photon energies above ~10 TeV allows the maximum particle acceleration energy to be inferred and implies that this unpulsed emission does not originate near the light cylinder of the pulsar but in the nebula, where the magnetic field is not strong enough to allow pair creation from the TeV photons. The hard gamma-ray energy spectrum above 10 TeV also provides information about the varying role of seed photons for the inverse Compton process at these high energies, as well as a possible contribution of pi deg gamma rays from proton collisions.
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