A detailed description of the asteroFLAG simulator will be presented elsewhere (Chaplin et al., in preparation). Here, we note briefly the main elements of the simulator. These elements are shown visually in block diagram form in Figure \[fig:sim\], with the simulator configured for observations made in intensity. Each timeseries comprises photometric perturbations from: p modes; granulation noise; active region noise; and photon shot and instrumental noise.

=12.5cm

### Fixing the input parameters {#sec:fixinputs}

We have used the Aarhus stellar evolution code (ASTEC) and the adiabatic pulsation code ADIPLS to compute theoretical adiabatic pulsation frequencies of the artificial stars (Christensen-Dalsgaard 2007a, b). We use results on stellar equilibrium and pulsation calculations, which have been applied in detail to the Sun and other Sun-like stars (Balmforth 1992; Houdek et al. 1999; Houdek & Gough 2002), to estimate the excitation rates and damping rates of the p modes. The amplitudes of the stochastically excited modes were obtained in the manner of Chaplin et al. (2005, 2007a).

Latitudinally dependent surface rates of rotation were fixed according to empirical laws, with scaling fixed by the colour, $B-V$, and age of the star (Aigrain, Favata & Gilmore 2005; Cardini & Cassatella 2007; Donahue et al. 1996; 