positions have been inferred using the traditional data (with the parallax for $m_v=9$). Here, we followed procedures the hounds would need to adopt to convert from absolute visual to absolute bolometric magnitude (we used the bolometric corrections of Flower 1996). The locations of the stars in Figure \[fig:where\] indicate that Pancho is intrinsically the brightest star; whilst Katrina is intrinsically the faintest star.

Figure \[fig:starpow\] shows how Kepler would see Pancho (left-hand panel), Boris (middle panel) and Katrina (right-hand panel), according to the asteroFLAG simulator, were the artificial stars to be observed continuously for 4yr at apparent visual magnitude $m_v=11$. Pancho shows the strongest p-mode amplitudes of the three stars, while Katrina has the weakest modes.

=6.0cm =6.0cm =6.0cm

Results
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The hounds made up six teams: JB, RAG and SJJ-R formed one team; while T. Arentoft, OC, STF, CR and DS worked individually. The hounds extracted estimates of the large frequency spacings using various methods. T. Arentoft used a Matched Filter approach, which is similar to methods applied in searches for exoplanet transits (see Christensen-Dalsgaard et al. 2007). The other hounds used either Fourier transforms of the power frequency spectra (one hound actually worked on autocorrelation functions of the 