  Swift J004929.5-733107 is an X-ray source in the Small Magellanic Cloud (SMC)
that has been reported several times, but the optical counterpart has been
unclear due to source confusion in a crowded region of the SMC. Previous works
proposed [MA93] 302 as the counterpart, however we show here, using data
obtained from the S-CUBED project, that the X-ray positio is inconsistent with
that object. Instead we propose a previously unclassified object which has all
the indications of being a newly identified Be star exhibiting strong HU
emission. Evidence for the presence of significant I-band variability strongly
suggest that this is, in fact, a Be type star with a large circumstellar disk.
Over 18 years worth of optical monitoring by the OGLE project reveal a periodic
modulation at a period of 413d, probably the binary period of the system. A
SALT optical spectrum shows strong Balmer emission and supports a proposed
spectral classification of B1-3 III-IVe. The X-ray data obtained from the
S-CUBED project reveal a time-averaged spectrum well fitted by a photon index =
0.93 pm 0.16. Assuming the known distance to the SMC the flux corresponds to a
luminosity 10E35 erg/s. All of these observational facts suggest that this is
confirmed as a Be star-neutron star X-ray binary (BeXRB) in the SMC, albeit one
with an unusually long binary period at the limits of the Corbet Diagram.
