to $W^+W^-$ near threshold and $b\bar{b}$ at $\lesssim 10$ GeV. Unfortunately, higher masses quickly become undetectable, particularly in the $W^+W^-$ case. If a convincing [$\overline{\text{D}}~$]{}signal is observed at GAPS or AMS-02, follow-up [$^3\overline{\text{He}}~$]{}observations may be needed to confidently rule out misidentified astrophysical secondaries.

There are two important technical instrumental differences in [$^3\overline{\text{He}}~$]{}detection compared to [$\overline{\text{D}}~$]{}which are not incorporated into our analysis. GAPS works by measuring X-ray cascades emitted during the formation of exotic atoms from antimatter and the gas target. This technique requires the particle to stop completely inside the detector, and the large volume and weight required could be prohibitive for satellite based missions. This also reduces the high-energy acceptance for heavier nuclei such as helium. Finally, searches at even lower energies increase the importance of geomagnetic field effects and would require a satellite very close to the geomagnetic poles.

Discussion and Conclusions {#sec:conclusions}
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Due to the low production rate of cosmic-ray anti-nuclei in interstellar proton-gas interactions, the observation of such particles remains an intriguing avenue for a positive signal from dark matter annihilation. We have, for the first time, modeled the production rates of $A=3$ cosmic-ray antinuclei by employing the [PYTHIA]{} event generator to reconstruct the angular 