If the maximum power recorded was not a *peak* inside the selected range, i.e. it lay at edge of the frequency range, then it was assumed to be leakage of power from a nearby and unrelated frequency. Whenever this situation occurred, the detection significance was set to zero since the probability that the power was due to the pulsar being searched for is negligible. For positive detections the pulse period and its uncertainty were also recorded. The uncertainty on the period was calculated using the formulation of [@kovacs1980] which accounts for the strength of the detected signal.

For each pulsar we only considered observations of duration greater than 4 pulsation cycles otherwise there are unacceptably large errors on the pulse period and poor confidence in their identification.

For each positive detection, the measured power $P_{LS}$ was converted into a pulse amplitude using Equation \[eqn:pow2amp\]: where the lightcurve has $N_P$ points and variance $\sigma^2$, the peak-to-valley amplitude (twice the sinusoidal amplitude) $A^{\ast}$ of a signal detected in the [Lomb-Scargle periodogram ]{}is: $$\label{eqn:pow2amp}
A^{\ast} = 4\sqrt {\frac{P_{LS} \sigma ^2}{N_P }}$$

The significance of peaks in the [Lomb-Scargle periodogram ]{}is described by a simple exponential function, related to the number of independent frequencies 