observational prospects at AMS-02 and GAPS have been thoroughly investigated (see e.g. [@donato2000; @profumo2005; @cui2010; @ibarraMC2013; @kadastik; @fornengo2013; @ibarra2013]). For an optimistic scenario of $\sim$100 GeV thermal WIMPs annihilating to $b \bar{b}$, the latter two state-of-the-art analyses predict $\mathcal{O}(0.1-10)$ [$\overline{\text{D}}~$]{}signal events – with backgrounds a factor $\mathcal{O}(10-50)$ smaller – to be measured by a GAPS Long Duration Balloon flight (LDB+). It is thus naively expected that the extremely low [$^3\overline{\text{He}}~$]{}flux will be difficult to observe. While this is likely to be true for upcoming experiments, a future satellite based mission could potentially probe this zero-background channel.

The outline of this letter is as follows. In Section \[sec:production\] we discuss the coalescence model for the production of [$^3\overline{\text{He}}~$]{}and calculate its formation rate relative to [$\overline{\text{D}}~$]{}. In Section \[sec:propagation\] we employ a simple diffusion model in order to calculate the expected flux of [$^3\overline{\text{He}}~$]{}at the solar position, and the penetration of [$^3\overline{\text{He}}~$]{}into the heliosphere. In Section \[sec:experiments\] we discuss flux scaling relations, calculate the flux, and discuss the possibility for [$^3\overline{\text{He}}~$]{}observation in both the current and upcoming AMS-02 and GAPS-LDB(+) experiments, as well as a future GAPS satellite mission. Finally in Section \[sec:conclusions\] we discuss the significance of our results to the 