Table 6
Best-fit solutions for the model tested in this work (quasi-periodic GP model) applied to the HARPS-N RV time series extracted with the DRS and TERRA pipelines.
| Jump parameter | Prior | Best-fit value | |
|---|---|---|---|
| DRS | TERRA | ||
| Stellar activity GP model | |||
| h (m s−1) |  (0,30) |
16.3 |
17.11 |
| λ (days) |  (0,1500) |
131 |
93 |
| w |  (0,1) |
0.33 |
0.33 ± 0.05 |
| θ (days) |  (0,20) |
16.99 |
17.06 ± 0.08 |
| σjit (m s−1) |  (0,20) |
2.5 ± 1.0 | 1.6 |
| γ (m s−1) |  (13550,13750) |
13640.7 |
−1.7 |
| Kb (m s−1) |  (0,10) |
2.1 ± 0.9 | 2.6 ± 0.7 |
| Kc (m s−1) |  (0,10) |
2.9 ± 1.1 | 3.4 ± 1.0 |
| Derived quantitiesa | |||
| mb (M⊕) | 3.2 |
3.9 ± 1.1 | |
| mc (M⊕) | 6.7 |
7.8 ± 2.3 | |
| ρb (g cm−3) | 5.9 |
7.2 |
|
| ρc (g cm−3) | 1.1 |
1.3 |
|
Bayesian Evidence  |
−301.45 ± 0.02 | −295.5 ± 0.08 | |
Notes. Our global model includes two orbital equations (circular and eccentric case). Uncertainties are given as the 16th and 84th percentiles of the posterior distributions. (a)Derived quantities from the posterior distributions. We used the following equations (assuming
Ms + mp≅Ms):
mp sin i ≅ (
;
, where
G is the gravitational constant. We set e = 0 for circular orbits.
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