Conservative constraints on dark matter annihilation into gamma rays

Abstract

Using gamma-ray data from observations of the Milky Way, Andromeda (M31), and the cosmic background, we calculate conservative upper limits on the dark matter self-annihilation cross section to monoenergetic gamma rays, $⟨{\ensuremath{\sigma}}_{A}v{⟩}_{\ensuremath{\gamma}\ensuremath{\gamma}}$, over a wide range of dark matter masses. (In fact, over most of this range, our results are unchanged if one considers just the branching ratio to gamma rays with energies within a factor of a few of the endpoint at the dark matter mass.) If the final-state branching ratio to gamma rays, $\mathrm{Br}(\ensuremath{\gamma}\ensuremath{\gamma})$, were known, then $⟨{\ensuremath{\sigma}}_{A}v{⟩}_{\ensuremath{\gamma}\ensuremath{\gamma}}/\mathrm{Br}(\ensuremath{\gamma}\ensuremath{\gamma})$ would define an upper limit on the total cross section; we conservatively assume $\mathrm{Br}(\ensuremath{\gamma}\ensuremath{\gamma})\ensuremath{\gtrsim}{10}^{\ensuremath{-}4}$. An upper limit on the total cross section can also be derived by considering the appearance rates of any standard model particles; in practice, this limit is defined by neutrinos, which are the least detectable. For intermediate dark matter masses, gamma-ray-based and neutrino-based upper limits on the total cross section are comparable, while the gamma-ray limit is stronger for small masses and the neutrino limit is stronger for large masses. We comment on how these results depend on the assumptions about astrophysical inputs and annihilation final states, and how GLAST and other gamma-ray experiments can improve upon them.