largely overlaps with the fields of view of the earlier observations. Position 3 was chosen to cover the eastern wing of the SMC which contains SMC X-1. Positions 2 and 4 were chosen to cover the rest of the SMC.

*Phase 3.* After 2 years of monitoring position 1, we broadened the search by shifting south to position 5, also in the main body of the SMC. The supplementary positions 2, 3 and 4 were not observed, as previous observations of these positions caused gaps in coverage of the main position. Position 5 was observed each week for 2.1 years.

Data Reduction Pipeline
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Data reduction was performed in two stages, “real-time monitoring” and “survey”: Immediately after each routine PCA observation, quick-look data were searched for new pulsars. Initially a lightcurve was generated at 3-10 keV and 0.1 second time resolution. No filtering criteria or background subtraction were applied at this stage. The power spectrum was inspected visually and with a peak search algorithm. This preliminary data analysis was usually performed within a day or so of the observation taking place, to identify new pulsars and schedule rapid TOO follow-up observations. The long-term survey made use of the production data, 