the majority of known pulsars in the SMC, these periods are given on the right of the plot. In addition to detecting pulse periods, this procedure also picks up harmonics and, in principle at least, low frequency quasi-periodic oscillations. In particular it has been observed in the course of this work that at times the $P_{pulse}/2$ harmonic can dominate the power spectrum. Therefore all significant power is included on the plots. The expected $P_{pulse}/2$ harmonics of known pulsars are indicated by dotted (green) lines. As the various pointing positions cover partially overlapping fields of view, different pulsars are visible in subsets of the data. Positions 1 and 5 comprise the bulk of the data.

Figure \[fig:peaks12345\] shows pulsars ranging in period from 0.7s (SMC X-1) to 755s (AX J0049.4-7323). It is immediately apparent that two sources were particularly active throughout the survey. The 172.4s and 323s pulsars appear to have undergone respectively 5 and 7 outbursts over a period of about 700 days. If these outbursts are normal Be/X-ray binary outbursts then the results are suggestive of orbital periods of (very) approximately 700/5=140d and 700/7=100d. The line labeled “2.37 & 2.39” is also of particular interest as the points lying 