  The content of matter in the Universe is estimated to be the 27% of its
critical density. It is almost universally accepted that most ot this matter is
non-baryonic. Constraints from primordial nucleosynthesis and cosmic background
radiation measurements impose that the baryonic content of the Universe cannot
exceed the 4% of the critical density, so the nature of the remaining 23% has
yet to be identi ed. In this sense, one of the most promising candidates is
represented by supersymmetric neutralinos. If they exist, they give rise to
relic densities in the required range, and are very well motivated in the
framework of theoretical extensions of the Standard Model of particle physics.
In addition to direct neutralino searches and collider experiments, neutralino
annihilation into gamma rays, neutrinos and synchrotron emission from the
charged products represents a reliable way of detecting these intriguing
particles. The strongest signals are expected to come from the Galactic Center
and from the nearest dwarf spheroidals. Clumps of dark matter in galactic
haloes are well predicted by high resolution cold dark matter numerical
simulations. In this work we present our studies on the gamma-ray emission from
the Galactic Center and from the Draco dwarf spheroidal. We investigate the e
ect of clumpiness on the detection of signals from neutalinos for di erent mass
density pro les. One of the scienti c goals of the MAGIC telescope are just
searches for the stable lightest supersymmetric particle in the di erent
physical scenarios in which they are produed. Assuming MAGIC speci cations, we
draw some conclusions about the potentialities of this telescope in such a kind
of investigation.
