to 1$\mu$s accuracy, and pulse-heights processed into 256 channels between 2-100 keV. According to the [*ABC of XTE*]{} the top layer of the PCA is the most sensitive, with the majority of source events occurring there, while the background rate is similar in all 3 layers. We verified that the detection significance for pulsars is slightly better using layer 1 only versus layers 1 and 2, when extracting lightcurves in the 2-10 keV band.

The program began after a new X-ray transient was detected during a PCA slew in the vicinity of SMC X-3 [@IAU6777]. A PCA observation was conducted on 1997 November 29 in response to this detection, revealing not SMC X-3 but three previously unknown pulsars with pulse periods of 91.s, 74s and 46.6s [@IAU6803]. Continued observations throughout December and January detected 2 more pulsars with periods of 169s [@IAU6814] and 58.9s [@IAU6818]. At times observations were being made at a rate of 1 per day, giving excellent temporal coverage of the outbursts of these pulsars. Following these observations, a program of regular monitoring was established (see Table \[tab:positions\]), with pointed PCA observations of several ksec duration made on a weekly basis. Pointing positions were carefully chosen to 