  The spectral distributions of Be/X-ray binaries in the Large Magellanic Cloud
and Galaxy have been shown to differ significantly from the distribution of
isolated Be stars in the Galaxy. Population synthesis models can explain this
difference in spectral distributions through substantial angular momentum loss
from the binary system. In this work we explore the spectral distribution of
Be/X-ray binaries in the Small Magellanic Cloud (SMC) using high
signal-to-noise spectroscopy of a sample of 37 optical counterparts to known
X-ray pulsars. Our results show that the spectral distribution of Be/X-ray
binaries in the SMC is consistent with that of the Galaxy, despite the lower
metallicity environment of the SMC. This may indicate that, although the
metallicity of the SMC is conducive to the formation of a large number of
HMXBs, the spectral distribution of these systems is likely to be most strongly
influenced by angular momentum losses during binary evolution, which are not
particularly dependent on the local metallicity.
