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   61070
   Shock acceleration is thought to be a common mechanism to generate high
   energy particle ensembles in astrophysical situation, but its nature is
   little understood due to the lack of the information of shock
   structures and particle distributions. SNR is the suitable object for
   getting the information up to 1E+14 eV, but we have too few samples of
   the acceleration to study systematically. To correct such samples, the
   hard X-ray information is essential, because the X-ray photons
   correspond to the synchrotron electron of 1E+14 eV in the typical
   magnetic field of shell-like SNRs. At this time, we search for samples
   in southern sky, where the air Cerenkov gamma-ray telescope can follow
   up, by which we can determine the magnetic field strength and the
   energy of the synchrotron electrons.
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