Astronomy & Astrophysics

Table 1: Accessible range of reduced orbital distance/planet effective temperature as a function of the spectral type of the parent star.
Table 2: Selection of expected detections for various planetary radii and reduced distances to the parent star/planet effective temperatures, assuming every star has one planet for such $a_{\rm r}$ and $R_{\rm P}$ . Figures are given for the entire mission and a confidence of less than one false detection. The crowding effect (Sect. 5.2) is expected to remove $\approx$ $10\%$ from the detections quoted here.
Table 3: Integrated number of detections for the entire mission as a function of the planetary radius (the confidence level corresponds to less than one false detection). The higher value corresponds to $a_{\rm r}^{\rm min} = 0.03$ AU and the lower to $a_{\rm r}^{\rm min} = 0.05$ AU. The crowding effect (Sect. 5.2) is expected to remove $\approx$ $10\%$ from the detections quoted here. The value for 10 $R_\oplus$ is given for completeness as the frequency of such planets is known to be much less than 1 planet per star per reduced AU.
Table 4: Impact of the stellar variability on the integrated number of detections expected for COROT. At the timescale of transits, the solar variability as estimated from SOHO data is $\simeq$ 50 ppm rms. The crowding effect (Sect. 5.2) is expected to remove $\approx$ $10\%$ from the detections quoted here.