(WIMP) dark matter, the pair-annihilation or decay of dark matter particles generically yields high-energy matter and antimatter cosmic rays. While the former are usually buried under large fluxes of cosmic rays of more ordinary astrophysical origin, antimatter is rare enough that a signal from dark matter might be distinguishable and detectable with the current generation of experiments. While astrophysical accelerators of high-energy positrons such as pulsars’ magnetospheres are well-known, observations of cosmic anti-nuclei might provide a unique window into physics beyond the Standard Model and may provide a discovery route to unveil the nature of particle dark matter.

Measurements of the cosmic-ray antiproton spectrum by BESS [@BESS; @BESS2; @BESS3] and PAMELA [@PAMELA_ANTIPROTON] currently provide the best limits on cosmic-ray antiprotons [$\bar{p}~$]{}in excess of the astrophysical background. On a short time-scale, AMS-02 will provide the most accurate cosmic-ray proton and antiproton spectrum to date, placing stringent limits on propagation parameters and excess signals. One well motivated origin for such an excess is the annihilation or decay of WIMPs to hadronic final states – generic to models coupling WIMPs to the weak gauge bosons or quarks (e.g. $W^+ W^-$ or $b\bar{b}$). While large astrophysical backgrounds often prohibit the clean disentanglement of exotic 