results for the frequency ranges chosen by a particular hound. The left-hand panel shows results from using the autocorrelation of the power frequency spectrum; while the right-hand panel shows results from using the Fourier transform of the power frequency spectrum. Agreement between the results is of course very good, so much so that it is hard to tell results apart for the autocorrelation method. However, there are differences present, which are in some cases as large as $\approx 0.75$% of the mean spacings. We consider below how scatter in the large spacing estimates translates to uncertainty in estimates of stellar radii.

=7.0cm =7.0cm

The main results on the large frequency spacings $\Delta\nu$ are shown for each star in Figures \[fig:panchores\], \[fig:borisres\] and \[fig:katrinares\]. The various symbols show results for different hounds. (JB, RAG and SJJ-R concentrated on developing application of the curvelet technique, and have returned results initially for Pancho only.) A first look at the results showed that there was no clear, systematic dependence of the estimated spacings on either the inclination or the internal rate of rotation. We therefore decided not to differentiate between these parameters when plotting the results (so that all estimates of $\Delta\nu$ for a 