to help fix suitable ranges in frequency to analyse. Furthermore, the curvelets used by JB, RAG and SJJ-R, certainly help in cleaning up the raw spectra to reveal the presence of any modes.

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Let us now turn to the main results. The top left-hand panel of each figure shows estimates of the large spacings returned by the hounds. The error bars show the uncertainties in $\Delta\nu$ required to give 1% uncertainties on the inferred radii of the stars. These values follow straightforwardly from the dependence of the mean spacing on the mean density of the star (e.g., Kjeldsen & Bedding 1995): $$\Delta\nu \propto M^{1/2}R^{-3/2}, 
 \label{eq:large1}$$ so that $$\delta R / R =-2/3 \delta \Delta\nu / \Delta\nu.
 \label{eq:large2}$$ The absolute uncertainty in $\Delta\nu$ required to give a 1% uncertainty in $R$ is therefore given by: $$\delta \Delta\nu_{1\,\%} = 0.01 \times 3/2 \Delta\nu = 0.015 \Delta\nu.
 \label{eq:large3}$$ The top right-hand panels of each figure again show estimates of the large spacings, but plotted over a much larger range on the ordinate to show poor estimates of the spacings.

The bottom left-hand panels of each figure show estimated spacings extracted (by 