WJC) from analysis of autocorrelations of noise-free power frequency spectra (see Figure \[fig:borislim\] and discussion above). The different symbols show results for the frequency ranges chosen by particular hounds. These results serve as a useful “noise-free” reference for the main (noisy timeseries) results shown in the top panels of each figure.

Finally, the bottom right-hand panels show estimates of the uncertainties on the large spacings returned by the hounds. The dashed lines show standard deviations of the results of the hounds at each apparent visual magnitude, $m_v$. The dotted lines again show the uncertainties in $\Delta\nu$ required to give 1% uncertainties on the inferred stellar radii. The most striking aspect of the uncertainty estimates is that they cover such a wide range.

Discussion {#sec:disc}
==========

How should we interpret the precision in the results (i.e., the observed scatter between hounds), and the uncertainty data plotted in the bottom right-hand panel of each figure? In reaching a conclusion we need to remember that all datasets on a given star had the same mode realization noise, but different shot noise.

At the brighter magnitudes (lower noise spectra), scatter between hounds is dominated by differences in implementation of the analysis (what we might 