hounds, we first illustrate the impact of some of the effects listed here.

We computed the smooth, noise-free “limit” power frequency spectrum of each timeseries, and then analysed each noise-free power frequency spectrum to estimate the large spacings. When we analysed each spectrum, we used the range in frequency that each hound chose when they analysed that same spectrum. We estimated the spacings using both of the basic methods adopted by the hounds. The results that are given correspond to a “best case scenario”, in that there is no noise in the power frequency spectrum. We note that our implementation of the methods most likely differed in detail from implementations of the hounds. The results provide a guide to differences we might expect from the free choice of the frequency range and analysis method, and of the inclination and mode frequency splittings. It is worth adding that the frequency range selected for analysis is information one would aim to use in determining the stellar radius, even if it was not possible to measure individual mode frequencies reliably.

Figure \[fig:borislim\] shows the estimated spacings extracted from noise-free power frequency spectra of the artificial star Boris. Each symbol is used to show 