and more detailed analysis methods. All data reduction was done with [*Ftools*]{}. Standard filtering criteria were applied to exclude data collected during: periods of high background; times when the source was attenuated by Earth’s atmosphere; during slews on/off source; and times immediately after SAA passage. On 2000 May 20 the upper propane veto-layer of PCU 0 was lost, after that date PCU 0 data were excluded. Filtering by detector/layer was performed with bit-masks generated by [*sefilter*]{}.

Background count-rates were generated using [*pcabackest*]{} and the L7 models for faint sources. Lightcurves and spectra were extracted from the generated background using [*saextrct*]{} with the same filtering criteria and detector/layer combinations as were applied to the science data.

### Lightcurve Extraction

Science lightcurves were extracted using [*seextrct*]{} at 0.01 second time binning for the 3-10 keV Good Xenon data from the top anode layer of each active PCU. This configuration maximizes signal-to-noise for pulsars. Background lightcurves were extracted with 16s binning (the minimum available) and subtracted from the science lightcurve, without modifying the errors on the science count-rates.

The lightcurve was then normalized to , by dividing each flux value by the number of PCUs active at that time. Lightcurve bin-times were corrected 