SMC X-2) have undergone a single giant outburst during our monitoring project. In these cases no orbital periods could be measured, instead pulse-period variations were used to constrain the contributions from orbital motion (Doppler shifts) and accretion torques.

Results I: Pulsar Monitor Charts {#sect:monitor}
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After reduction, the data were analyzed in 2 separate ways to search for variable sources, the first of these is the blind search.

Having generated the [Lomb-Scargle periodogram ]{}for every observation, the resulting database of periodograms was searched for significant peaks. The significance level for each observation was estimated individually. This stage was executed as a “blind search”, the threshold adopted was 90% significance considering all frequencies in the (period) range 0.5 -1000 seconds. We used a simple boxcar peak-search algorithm which identified a peak as any frequency having a greater power than its nearest neighbors, subject to that power being above the 90% significance level. Figure \[fig:peaks12345\] displays the combined results of this analysis in the form of a “pulsar activity monitor”, showing the activity of bright pulsars in all the monitoring positions. The size of the graph markers indicates spectral power on a logarithmic scale, horizontal dashed lines (red) indicate pulse periods of 