  The observations suggest that $\gamma$-ray bursts (GRBs) are produced by jets
of relativistic cannonballs (CBs), emitted in supernova (SN) explosions. The
CBs, reheated by their collision with the SN shell, emit radiation and
Doppler-boost it to the few-hundred keV energy of the GRB's photons.
Chaperoning the GRB, there should be an intense flux of neutrinos of a few
hundreds of GeV energy, made in $\pi^\pm$ decays: the SN shell acts as a dump
of the beam of CBs. The $\nu$ beam carries almost all of the emitted energy,
but is much narrower than the GRB beam and should only be detected in
coincidence with the small fraction of GRBs whose CBs are very precisely
pointing to us. The $\pi^0$s made in the transparent outskirts of the SN shell
decay into energetic $\gamma$-rays (EGRs) of energy of ${\cal{O}}$(100) GeV.
The EGR beam, whose energy fluence is comparable to that of the companion GRB,
is as wide as the GRB beam and should be observable, in coincidence with GRBs,
with existing or planned detectors.
