radii of the artificial stars, using the estimated spacings as one of the key data inputs.

When mode peaks observed in the power frequency spectra are of sufficient quality it will be possible to obtain extremely precise estimates of *individual* mode frequencies, for example by application of peak-bagging fitting methods developed for Sun-as-a-star data. Use of individual mode frequencies will then allow even tighter constraints to be placed on the stellar radii, and we will also test such analyses using the artificial asteroFLAG datasets.

Our intention is to provide input and guidance to the KASC to help develop a robust strategy, or recipe, for estimation of stellar radii under different dataset scenarios (i.e., for different intrinsic stellar properties and noise levels). In this paper we show initial results from Exercise\#1 on estimation of the large spacings. WJC and four other colleagues (T. Appourchaux, GH, RN and TS) have thus far acted as the hares, and have generated artificial data on a selection of main-sequence stars for other members of the group, the hounds, to analyse blind. The hounds who have returned results thus far are T. Arentoft, JB, OC, STF, RAG, SJJ-R, CR and DS.

The asteroFLAG simulator {#sec:sim}
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