  In the frame of indirect dark matter searches we investigate the flux of
high-energy $\gamma$-ray photons produced by annihilation of dark matter in
caustics within our Galaxy under the hypothesis that the bulk of dark matter is
composed of the lightest supersymmetric particles. Unfortunately, the detection
of the caustics annihilation signal with currently available instruments is
rather challenging. Indeed, with realistic assumptions concerning particle
physics and cosmology, the $\gamma $-ray signal from caustics is below the
detection threshold of both $\check {\rm C}$erenkov telescopes and
satellite-borne experiments. Nevertheless, we find that this signal is more
prominent than that expected if annihilation only occurs in the smoothed
Galactic halo, with the possible exception of a $\sim 15^{\circ}$ circle around
the Galactic center if the mass density profile of our Galaxy exhibits a sharp
cusp there. We show that the angular distribution of this $\gamma$-ray flux
changes significantly if DM annihilation preferentially occurs within
virialized sub-halos populating our Galaxy rather than in caustics.
