  In this letter, we suggest that a nearby clump of 600-1000 GeV neutralinos
may be responsible for the excesses recently observed in the cosmic ray
positron and electron spectra by the PAMELA and ATIC experiments. Although
neutralino dark matter annihilating throughout the halo of the Milky Way is
predicted to produce a softer spectrum than is observed, and violate
constraints from cosmic ray antiproton measurements, a large nearby (within 1-2
kiloparsecs of the Solar System) clump of annihilating neutralinos can lead to
a spectrum which is consistent with PAMELA and ATIC, while also producing an
acceptable antiproton flux. Furthermore, the presence of a large dark matter
clump can potentially accommodate the very large annihilation rate required to
produce the PAMELA and ATIC signals.
