  The Small Magellanic Cloud (SMC) is well known to harbor a large number of
High-Mass X-ray Binaries (HMXBs). The identification of their optical
counterparts provides information on the nature of the donor stars and can help
to constrain the parameters of these systems and their evolution. We obtained
optical spectra for a number of HMXBs identified in previous Chandra and
XMM-Newton surveys of the SMC using the AAOmega/2dF fiber-fed spectrograph at
the Anglo-Australian Telescope. We find 5 new Be/X-ray binaries (BeXRBs;
including a tentative one), by identifying the spectral type of their optical
counterparts, and we confirm the spectral classification of an additional 15
known BeXRBs. We compared the spectral types, orbital periods, and
eccentricities of the BeXRB populations in the SMC and the Milky Way and we
find marginal evidence for difference between the spectral type distributions,
but no statistically significant differences for the orbital periods and the
eccentricities. Moreover, our search revealed that the well known supergiant
B[e] star LHA 115-S 18 (or AzV 154) is associated with the weak X-ray source
CXOU J005409.57-724143.5. We provide evidence that the supergiant star LHA
115-S 18 is the optical counterpart of the X-ray source, and we discuss
different possibilities of the origin of its low X-ray luminosity (Lx ~ 4 x
10^33 erg/s).
