minus the net pointing offset in degrees. Values of [*R*]{} for each pulsar in each of the monitoring positions are listed in Table \[tab:responses\]. This table should be consulted when examining the long-term pulsar lightcurves in Section \[sect:lcurves\]. It is apparent that the scatter in flux measurements is correlated with $R$. Blank entries in Table \[tab:responses\] indicate that the pulsar was not in the field of view. In practice, observations at marginal sensitivity were also excluded. A value of $R < 0.1$ was regarded as marginal and a lightcurve not extracted for observations of that particular pulsar/pointing position combination. For spectral analysis in this paper we utilize the full detailed model of collimator response for those sources with accurate positions.

Timing Analysis
---------------

The methods used to measure pulse periods, pulse amplitudes, calculate significance levels and reject false detections are outlined here.

A [Lomb-Scargle periodogram ]{}[@Scargle82] was calculated for each observation, scanning the range 0.02-1000 s at a resolution of $1\times 10^{-5}$ Hz. Also generated by the pipeline were statistical parameters used in assigning significance levels and converting between spectral power and pulsed flux.

The special properties of the [Lomb-Scargle periodogram ]{}were exploited to scan every observation around the period 