Collider search

Indirect Detection

Direct Detection

7 TeV proton + 7 TeV proton

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

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

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

The detection depends on WIMP properties DM distributions around the center Astrophysical foreground

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.

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.

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