  On MJD 56590-1 (2013 Oct 25-26) observations of the Magellanic Clouds by the
INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) observatory
discovered a previously-unreported bright, flaring X-ray source. This source
was initially given the identification IGR J00569-7226. Subsequent
multi-wavelength observations identified the system as new Be/X-ray binary
system in the Small Magellanic Cloud. Follow-up X-ray observations by Swift and
XMM-Newton revealed an X-ray pulse period of 5.05s and that the system
underwent regular occulation/eclipse behaviour every 17d. This is the first
reported eclipsing Be/X-ray binary system in the SMC, and only the second such
system known to date. Furthermore, the nature of the occultation makes it
possible to use the neutron star to X-ray the circumstellar disk, thereby, for
the first time, revealing direct observational evidence for its size and clumpy
structure. Swift timing measurements allowed for the binary solution to be
calculated from the Doppler shifted X-ray pulsations. This solution suggests
this is a low eccentricity binary relative to others measured in the SMC.
Finally it is interesting to note that the mass determined from this dynamical
method for the Be star (approx 13 solar masses) is significantly different from
that inferred from the spectroscopic classification of B0.2Ve (approx 16 solar
masses) - an effect that has been noted for some other high mass X-ray binary
(HMXB) systems.
