region. All of these observations are included in the long-term lightcurve (Figure \[fig:smcx2amp\]).

The duration of the outburst was constrained by non-detections before and after the dates given in Table \[tab:x2flux\], on MJD 51560 and 51666-7 and 51670. The upper limits for the end of the outburst are more stringent as these observations were pointed directly at the position of SMC X-2.

Due to changes is the power spectrum of SMC X-2 during the outburst, pulse periods were refined by PDM [@Stellingwerf78]. The refined periods are given in Table \[tab:x2flux\]. The pulse profiles (Figure \[fig:x2pro\]) obtained during the outburst show an interesting trend with luminosity. During the low luminosity observations at the beginning and end of the outburst, the pulse profile was a weakly double peaked shape, with roughly equal peaks separated by half a cycle: typical of that seen in many X-ray pulsars. At high luminosity the shape changed, with peak flux occurring either side of a narrow minimum, the separation between the first and second peak now 0.7 in phase. This change was seen in the power spectra as a reversal in the normal ratio of the fundamental and 1st harmonic: evident from the pulsar monitor (Figure \[fig:peaks12345\]) 