this may have been because those estimates came from standard least-squares fits to autocorrelations of the power frequency spectra, where no account had been taken of the strong correlations present in the autocorrelation functions. (See also Chaplin et al. 2007b, for discussion of a similar problem, using the cross correlation function.)

Conclusion {#sec:conc}
==========

The following conclusions may be drawn from the results:

1.  It is possible to extract robust estimates of the large frequency spacings, $\Delta\nu$, for many of the timeseries we made. Estimated spacings of the different hounds, returned at values of apparent visual magnitude where robust estimation is possible, show agreement at a level typically better than 1%.

2.  The observed level of agreement implies a contribution to the uncertainty on inferred stellar radii of typically a few tenths of 1%.

3.  Scatter in the results increases significantly at $m_v=15$ for Pancho; at $m_v \ge 13$ for Boris; and at $m_v > 9$ for Katrina. Indeed, for the intrinsically fainter Katrina no results on the spacings were returned at $m_v \ge 11$.

4.  The observed scatter between hounds for the brighter stars tends to be larger than the characteristic internal precision expected, given the intrinsic quality of 