dark matter annihilations in the halo of the Milky Way, galactic substructure and the dark matter distribution integrated over cosmological volumes. In this section, we briefly describe the role of these experimental programs in the overall strategy to reveal dark matter’s identity.

Gamma Rays
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Searches for prompt photons generated in dark matter annihilations have a key advantage over other indirect detection channels in that they travel essentially unimpeded from their production site. In particular, gamma rays are not deflected by magnetic fields, and thus can potentially provide valuable angular information. For example, point sources of dark matter annihilation radiation might appear from high density regions such as the Galactic Center or dwarf spheroidal galaxies. Furthermore, over galactic distance scales, gamma rays are not attenuated, and thus retain their spectral information. In other words, the spectrum observed at Earth is the same spectrum that was generated in the dark matter annihilations.

The spectrum of photons produced in dark matter annihilations depends on the details of the WIMP being considered. Supersymmetric neutralinos, for example, typically annihilate to final states consisting of heavy fermions and gauge or Higgs bosons [@jungman]. Generally speaking, each of these annihilation modes typically result in a very 