Gamma-ray binaries are a small subclass of high-mass binaries containing an O or B/Be star and a
compact object. These systems produce non-thermal emission across all wavelengths but peak at
energies greater than 1 MeV. In order to interpret the source of the non-thermal emission in these
systems, an orbital solution is required. The gamma-ray binary HESS J0632+057, which consists
of a Be star and an unidentified compact object, still lacks a clear orbital solution; complicating
the interpretation of the modulated emission, despite previous attempts to constrain the orbital
parameters. Two different and incompatible solutions were proposed by Casares et al. 2012 and
Moritani et al. 2018 - through radial velocity measurements of the absorption lines and the H 𝛼
emission line respectively. In order to better constrain the orbital solution, we are undertaking
independent radial velocity measurements using the HRS with SALT of both the weak absorption
lines and the H 𝛼, H 𝛽, and H 𝛾 emission lines. We present the initial results from our first two
semesters of observations.