Table 4
P-values for the different coefficients used in Eq. (5) for the correction of stellar activity induced by an equatorial 1% spot on the simulated Sun, and a planet with a period of one-third the rotational period of the star and a semi-amplitude of 10 m s−1.
| Parameter | N mean RV | SN mean RV | SN median RV |
|---|---|---|---|
| β0 | 0.95 | 0.076 | 0.21 |
| β1 | 0.0020 | 0.11e − 4 | 0.12e − 4 |
| β2 | 2.22e − 16 | 2.22e − 16 | 2.22e − 16 |
| β3 | 0.92 | 0.60 | 0.61 |
| β4 | 0.34 | 0.27 | 0.27 |
| K | 2.22e − 16 | 2.22e − 16 | 2.22e − 16 |
| P | 2.22e − 16 | 2.22e − 16 | 2.22e − 16 |
| t0 | 2.22e − 16 | 2.22e − 16 | 2.22e − 16 |
| Residuals | 2.80 m s−1 | 2.29 m s−1 | 2.29 m s−1 |
Notes. All the parameters corresponding to the Normal or SN variables are statistically significant, except the intercept β0, width of the CCF β3, and interaction term β4 that evaluates the interaction between the width and asymmetry of the CCF. Once corrected for stellar activity andthe presence of the planet, the residuals are smaller in terms of rms when using the SN variables. We note that because we used nonlinear least squares to fit the best model, the residual rms rather than the R2 is listed as a reference.
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