  The prediction of isotopic abundances resulting from the rapid neutron
capture process (r-process) requires high-precision mass measurements. Mass
measurements of $^{79-83}$Zn and $^{85,86}$Ga using TITAN's on-line
time-of-flight spectrometer. First time measurements are performed for
$^{79m}$Zn, $^{83}$Zn, and $^{86}$Ga. These measurements reduced uncertainties,
and are used to calculate isotopic abundances near the first r-process
abundance peak using astrophysical conditions present during a binary neutron
star (BNS) merger. Good agreement across a range of trajectories is found when
comparing to several metal-poor stellar abundances. Particularly, this subset
of trajectories produces agreement with the abundance pattern of both the
`r/s-star' HD94028 as well as the `r-process star' HD222925. These findings
point to a high degree of sensitivity to the electron fraction of a BNS merger
on the final elemental abundance pattern near the first r-process peak. In
particular, we find that small changes in electron fraction produce distinct
abundance patterns that match those of metal-poor stars with different
classifications, calls the need for an i-process into question.
