An analysis of the X-ray and optical observations was presented by @Laycock02b identifying a possible B0V-B1V counterpart. No additional outbursts were detected, as evidenced by Figure \[fig:4.78amp\]. For most of the outburst the pulse profile was strongly double peaked, causing the $P_{pulse}/2$ harmonic power to be more indicative of the actual pulsed flux, a feature that is evident in the pulsar monitor (Figure \[fig:peaks12345\]). In all cases around the time of the outburst, the amplitude of the $P/2$ harmonic in Figure \[fig:4.78amp\] was plotted if it was greater than the fundamental.

2E 0050.1-7247 (8.88s)
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The pulsar activity monitor (Figure \[fig:peaks12345\]) shows two strong detections of a $\sim$9 second pulsar which appear to correspond to the 8.88s pulsar 2E 0050.1-7247. The pulsed flux history reveals a number of detections in 3 groups separated by $\approx$ 200 days. Although some of the detections appear to at least roughly coincide with detections of the 16.6s pulsar the uncertainties on our period determinations apparently exclude the possibility that pulsations at 8.88s are harmonics of the 16.6s source. A 2-10 keV pulse profile obtained during the brightest detection of 8.88s pulsations is shown in Figure \[fig:8.88pro\], it is triple peaked.

RX J0052.1-7319 (15s)
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