but one may simply rescale dN/dE (or the final flux presented later) by a factor $(1+\epsilon)/2$ to regain full generality. We note that this uncertainty is small compared to the weakly constrained coalescence momentum.

In Figure \[fig:ratios\] we show ratios of the [$^3\overline{\text{He}}~$]{}to [$\overline{\text{D}}~$]{}injection spectra integrated over the energy band 0.1-0.25 GeV/n relevant for the upcoming GAPS Long Duration Balloon Flights (LDB and LDB+) as a function of the $A=2$ and $A=3$ coalescence momenta, for four different combinations of the dark matter pair-annihilation final state ($b\bar b$ in the left panels, $WW$ in the right panels) and mass (10, 1000 and 2000 GeV). The GAPS energy bands are quoted for kinetic energies at the top of Earth’s atmosphere, after the particle momenta have been shifted by propagation through the heliosphere. Solar modulation will be discussed in detail in Section \[sec:propagation\], but for concreteness, we integrate the [$^3\overline{\text{He}}~$]{}and [$\overline{\text{D}}~$]{}yields over bands shifted according to a Fisk potential of 500 MV in Figure \[fig:ratios\].

The uncertainties on the coalescence momentum for $A=2$ are represented by the vertical shaded bands. For $A=3$ coalescence momenta, the two horizontal lines in each panel represent scaling with the binding energy (blue-dashed line) and heavy-ion collisions (black 