give good coverage of the main body of the SMC, as shown in Figure \[fig:smcpic\]. The “wing” was not regularly observed due to the presence of the luminous supergiant High-Mass X-ray Binary (HMXB) SMC X-1. This source was deliberately excluded from the PCA survey because its persistent emission, very strong pulsations, and timing noise mask the presence of other weaker pulsars when it is in the field of view. Observations were made in 3 phases during which slightly different observing strategies have been employed, as described below.

*Phase 1.* This comprises the series of observations conducted and described by @Lochner99a. The observations were made primarily in two positions designated 1a and 1c. Position 1a was centered on the location of SMC X-3, because the initial source detected was at first thought to be SMC X-3. Position 1b was the position of a single PCA pointing aimed at the location of one of the new pulsars. Position 1c lies close by and was used throughout 1998 to monitor the activity of the 4 newly discovered pulsars mentioned above.

*Phase 2.* During this period we continued to monitor the known pulsars and at the same time search for new sources. Position 1 