2. Collider searchIndirect Detection Direct Detection

3.  7 TeV proton + 7 TeV proton

4.  If Dark Matter has weak interactions and its mass is less than 3-5TeV, they can be pair-produced at LHC

5. Dark Matter can be annihilated in space, producing ordinary matter  Electron-positron pair, quark-antiquark pair  High-energy X-ray ， gamma ray, and neutrinos

6.  Gamma provides direct profile of the DM annhilation.  Gamma spectrum depends on the final state SM particles

8.  The detection depends on  WIMP properties  DM distributions around the center  Astrophysical foreground

14.  PAMELA and ATIC observations suggest the presence of a relatively local (within ∼ 1 kpc) source or sources of energetic cosmic ray electrons and positrons.  WMAP experiment has revealed an excess of microwave emission from the central region of the Milky Way which has been interpreted as synchrotron emission from a population of electrons/positrons with a hard spectral index.  The interpretations of the observations have focused two possibilities: emission from pulsars, and dark matter annihilations  A large fraction of the annihilations must proceed to electron- positron pairs, or possibly to μ+μ− or τ+τ−. Furthermore, WIMPs annihilating to other final states typically exceed the observed flux of cosmic ray antiprotons if normalized to generate the PAMELA and ATIC signals.

16.  Due to gravitational potential, the DM density in the sun is much larger than average. DM particles get trapped after collisions, loosing their kinetic energy  DM particles can annihilate into neutrinos, with energy equaling to the mass of these particles  GeV-TeV scale neutrinos can travel out of the sun and get detected.

17.  Using a 1km cube of ice 1km below the surface to detect high-energy neutrinos  The neutrinos come from the deep earth, and scatter with matter particle, producing muon  A + ν  A* + µ