  The details of what constitutes the majority of the mass that makes up dark
matter in the Universe remains one of the prime puzzles of cosmology and
particle physics today - eighty years after the first observational
indications. Today, it is widely accepted that dark matter exists and that it
is very likely composed of elementary particles - that are weakly interacting
and massive (WIMPs for Weakly Interacting Massive Particles). As important as
dark matter is in our understanding of cosmology, the detection of these
particles has so far been elusive. Their primary properties such as mass and
interaction cross sections are still unknown. Indirect detection searches for
the products of WIMP annihilation or decay. This is generally done through
observations of gamma-ray photons or cosmic rays. Instruments such as the
Fermi-LAT, H.E.S.S., MAGIC and VERITAS, combined with the future Cherenkov
Telescope Array (CTA) will provide important and complementary constraints to
other search techniques. Given the expected sensitivities of all search
techniques, we are at a stage where the WIMP scenario is facing stringent tests
and it can be expected that WIMPs will be either be detected or the scenario
will be so severely constrained that it will have to be re-thought. In this
sense we are on the "Threshold of Discovery". In this article, I will give a
general overview over the current status and the future expectations for
indirect searches for dark matter (WIMP) particles.
