realization noise was always used to excite the overtones of each ($l,m$) of a given star, regardless of the dataset; however, different realizations of the photon shot noise were added at each of the different apparent magnitudes. As indicated previously, the timeseries did not include stellar-cycle-like effects.

These multiple timeseries were intended to help the hounds test their analysis codes, and so the hares also passed to the hounds a priori information on the inclinations and rotation rates of the datasets. It is in the next phase of Exercise\#1 that data will be released at only one $m_v$ per star, on a selection of new stars, thereby providing true blind tests for the hounds. We comment below on the potential impact on the results of the additional a priori information given by having multiple timeseries on each star.

=8.3cm

In addition to the timeseries data, the hares also released ‘traditional’ data on the stars, appropriate to each apparent visual magnitude, $m_v$. The traditional data were: parallaxes, $\pi$, metallicities, \[Fe/H\], and effective temperatures, $T_{\rm eff}$. (Full details on these data will be given in a separate paper.) Figure \[fig:where\] shows the location of the artificial stars on a temperature-luminosity diagram. The 