  The problem of the dark matter in the universe is reviewed. A short history
of the subject is given, and several of the most obvious particle candidates
for dark matter are identified. Particular focus is given to weakly
interacting, massive particles (WIMPs) of which the lightest supersymmetric
particle is an interesting special case and a usful template. The three
detection methods: in particle accelerators, by direct detection of scattering
in terrestrial detectors, and indirect detection of products from dark matter
particle annihilation in the galactic halo, are discussed and their
complementarity is explained. Direct detection experiments have revealed some
possible indications of a dark matter signal, but the situation is quite
confusing at the moment. Very recently, also indirect detection has entered a
sensitivity region where some particle candidates could be detectable. Indeed,
also here there are some (presently non-conclusive) indications of possible
dark matter signals, like an interesting structure at 130 GeV gamma-ray energy
found in publicly available data from the Fermi-LAT space detector. The future
of the field will depend on whether WIMPs are indeed the dark matter, something
that may realistically be probed in the next few years. If this exciting
scenario turns out to be true, we can expect a host of other, complementary
experiments in the coming decade. If it is not true, the time scale and methods
for detection will be much more uncertain.
