tabulated in Ref. [@prop_model]. The resulting uncertainty in the flux spans three orders of magnitude. However, the [$\overline{\text{D}}~$]{}and [$^3\overline{\text{He}}~$]{}fluxes are tightly correlated to [$\bar{p}~$]{}whose flux is well measured by PAMELA. The propagation uncertainty on the *maximal* [$\overline{\text{D}}~$]{}(and [$^3\overline{\text{He}}~$]{}) flux allowed by the measured $p$/[$\bar{p}~$]{}ratio is then reduced to within a factor 4 of the MED model [@ibarra2013][^1]. Upcoming antiproton results from AMS-02 will tighten this upper-limit and the large nuclear physics will certainly dominate in the case of antihelium. In particular, the [$^3\overline{\text{He}}~$]{}flux is sensitive to the sixth power of $p_0^{A=3}$, making updated collider production rates for [$\overline{\text{D}}~$]{}and [$^3\overline{\text{He}}~$]{}a crucial factor in *any* estimate of an anti-nucleon flux.

The flux at the solar system is found by numerically integrating the dark matter annihilation rates over the dark matter halo and solving the transport equation analytically. For local dark matter density $\rho_\odot$, dark matter mass $m_\chi$, and thermal cross-section $\langle \sigma v \rangle$, the antihelium flux at the boundary of the solar system is given by $$\begin{aligned}
\label{eq:pnum}
\begin{split}
\Phi^{\mathrm{IS}}_{\overline{He}} (T)= \left(\frac{\rho_0}{0.39~\mathrm{GeV cm}^{-2}}\right)^2 \left(\frac{100~\mathrm{GeV}}{m_\chi}\right)^2\\
\times \left(\frac{\langle \sigma v\rangle}{3\times 10^{-26} \mathrm{cm}^3/\mathrm{s}}\right) \cdot P_{\mathrm{num}}(T) \cdot \frac{dN(T)}{dT},
\end{split}\end{aligned}$$ where $P_{\mathrm{num}}(T)$ is the energy dependent numerical output of the propagation code and dN/dT is the 