Download Dark Matter and Its Direct Detection

Direct Detection
Collider search
Indirect Detection
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7 TeV proton + 7 TeV proton
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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
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Gamma provides direct profile of the DM annhilation.
Gamma spectrum depends on the final state SM particles
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The detection depends on
 WIMP properties
 DM distributions around the center
 Astrophysical foreground
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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 electronpositron 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
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.
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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