Table 4.
Best-fit values for the parameters of the global model (one planet on a circular orbit + stellar activity) selected as explained in Sect. 5.
| Parameter | Value | Prior |
|---|---|---|
| (planet) | ||
| Kb ( m s−1) |  |
 (0,20) |
| Pb (days) |  |
 (13.5, 17.5) |
| T0,b (BJD-2450000) |  |
 (7800, 7820) |
| e | 0 (fixed) | – |
| (hyper)parameter | Value | Prior |
| (stellar activity) | ||
| h HARPS ( m s−1) |  |
 (0,20) |
| h HIRES ( m s−1) |  |
 (0,20) |
| λ (days) |  |
logλ  (0,3.9) |
| w |  |
 (0,1) |
| θ (days) |  |
 (0, 50) |
| offset_HARPS-N ( m s−1) |  |
 ( − 100, 100) |
| σjitter,HARPS-N ( m s−1) |  |
 (0, 10) |
| offset_HARPS ( m s−1) |  |
 ( − 100, 100) |
| σjitter,HARPS ( m s−1) |  |
 (0, 10) |
| offset_HIRES ( m s−1) |  |
 ( − 100, 100) |
| σjitter,HIRES ( m s−1) |  |
 (0, 10) |
| Derived quantities | ||
| Mb sini (M⊕) | 7.1 ± 0.9 | |
| ab (AU) | 0.091 ± 0.004 | |
| Teq, b (K) | 379 |
|
Notes.
The parameters are calculated as medians of the marginal posterior distributions, and the uncertainties represent their 16 and 84% quantiles, unless otherwise indicated. The priors used in our MC fitting are also shown. The difference
between theBayesian evidence for this model and the one for a “null” model not including a planet is
, which indicates decisive evidence in favor of the one-planet model according to Kass & Raftery (1995). For the “null” model we fitted the data only through a GP quasi-periodic regression, using the same priors for the hyper-parameters as for the one-planet model. The symbol
(⋅,⋅) denotes an uninformative prior with corresponding lower and upper limits. The equilibrium temperature
Teq,b was derived by assuming Bond albedo AB = 0.
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