this paper. While we have performed 19 independent experiments and found only 1 detection we point out that of our 19 data sets only 7 have average counts (Table 1) equal to or more than the observation in which we find the QPO. One cannot expect to see with equal likelihood, a periodicity of equal strength in these weaker AGN.

We note that independently, the XWT finds evidence for power throughout the observation at 3.3 ks (Fig. 8). We measured the 3.3 ks signal strength across the time series from the power plot of Figure 8. The power of the 3.3 ks signal is $\sim$ 4000 times stronger than shorter and longer dilations, illustrating that the 3.3 ks period is well-constrained. We also ran the XWT on this time series with analyzing signals of 2.3 ks and 4.3 ks. The average power of these signals is $\sim$ 2 times less than the average power of the 3.3 ks signal. This demonstrates that the XWT is picking out a well-defined, persistent signal, and will not misleadingly suggest a signal where there is none.

We did not find any significant detections for the other nine AGN in our sample. No features had 