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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 beenunclear due to source confusion in a crowded region of the SMC. Previous worksproposed [MA93] 302 as the counterpart, however we show here, using dataobtained from the S-CUBED project, that the X-ray positio is inconsistent withthat object. Instead we propose a previously unclassified object which has allthe indications of being a newly identified Be star exhibiting strong HUemission. Evidence for the presence of significant I-band variability stronglysuggest 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 periodicmodulation at a period of 413d, probably the binary period of the system. ASALT optical spectrum shows strong Balmer emission and supports a proposedspectral classification of B1-3 III-IVe. The X-ray data obtained from theS-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 aluminosity 10E35 erg/s. All of these observational facts suggest that this isconfirmed as a Be star-neutron star X-ray binary (BeXRB) in the SMC, albeit onewith an unusually long binary period at the limits of the Corbet Diagram.

The Be/neutron star system Swift J004929.5-733107 in the Small Magellanic Cloud -- X-ray characteristics and optical counterpart candidates