of different overtones, coupled with the later addition of granulation noise to the p-mode timeseries, gave rise to asymmetries of the resonant peaks in the power frequency spectrum (asymmetries that are displayed by the solar p modes).

To give an idea of the expected quality of the Kepler observations, Figure \[fig:sun09\] shows how Kepler would see the Sun, according to the asteroFLAG simulator, were the Sun to be observed continuously for 4yr at apparent visual magnitude $m_v=9$. This is at the bright $m_v$ end of the target range, which extends down to brightness $m_v
\sim 15$ (e.g., Christensen-Dalsgaard et al. 2007).

=9.0cm

Data for Exercise\#1 {#sec:data}
--------------------

For the first phase of Exercise\#1, we have prepared timeseries of Kepler-like data on 3 artificial stars. We have named the artificial stars Pancho, Boris and Katrina[^2] Here, we present results on a total of twenty-eight 4-yr timeseries prepared for each star. These timeseries covered all possible combinations of the following:

-   Four different apparent visual magnitudes, $m_v=9$, 11, 13 and 15;

-   Three different angles of stellar inclination, $i=0$, 30 and 60 degrees;

-   Three different mean internal rates of rotation: Sun-like, twice Sun-like, and three-times Sun-like;

We note that the same 