given star are plotted on the same graph).

It is important to recognise that choices made for the higher noise (larger $m_v$) spectra may have been influenced by results on the lower noise (smaller $m_v$) spectra. Perhaps the most important choice is the part of the power frequency spectrum that is selected for subsequent analysis. The choice can be less than straightforward when the mode peaks are not readily apparent in the power frequency spectrum. Under such circumstances it may still be possible to extract a robust estimate of the spacing provided the right part of the spectrum is selected. This is the most obvious example of where our hounds will have learned from, and therefore benefited by, their selections made for the lower noise spectra.

We should add that information included with the results returns (together with the results themselves) suggests that the hounds did attempt to treat each timeseries on its own merits. But this may not always have been possible where the choice of frequency range was concerned. For analysis on real stars, and in the absence of prominent mode peaks in the power frequency spectrum, one would seek to use already-known traditional information on the star 