sources, a recent analysis projects that the 1-year AMS-02 data will produce robust constraints on WIMP annihilation to heavy quarks below the thermal-relic cross-section for dark matter masses $30 \leq m_{\chi} \leq 200 $ GeV [@antiproton2].

In addition to antiprotons, Ref. [@donato2000] proposed new physics searches using heavier anti-nuclei such as antideuteron ([$\overline{\text{D}}~$]{}), antihelium-3 ([$^3\overline{\text{He}}~$]{}), or antitritium ([$^3\overline{\text{H}}~$]{}) forming from hadronic neutralino annihilation products. Although such production is of course highly correlated with the antiproton spectrum, the secondary astrophysical background decreases much more rapidly than the expected signal as the atomic number $A$ is increased [@duperray2005]. In particular, secondary antinuclei production from the spallation of high-energy cosmic rays – i.e. the scattering of cosmic-ray protons off of cold interstellar hydrogen and helium – quickly becomes kinematically suppressed for heavier nuclei for three reasons:

\(i) the constituent nucleons must lie in a small volume of phase space in order to form anti-nuclei, leading to a production suppression of roughly $10^{2A}-10^{3A}$. While this is the case for both primary (e.g. dark matter) and secondary anti-nuclei, the secondary background is further suppressed by the rapid falloff of cosmic-ray protons at high energies. The dominant spallation processes which generate [$\bar{p}~$]{}, $\overline{\text{D}}$, and [$^3\overline{\text{He}}~$]{}/[$^3\overline{\text{H}}~$]{}have production 