Table 3
Best-fit solutions for the quasi-periodic GP model applied to the combined HARPS/HARPS-N RV time series extracted with TERRA and an alternative pipeline.
| Jump parameter | Best-fit value | |
|---|---|---|
| TERRA | alternative pipeline | |
| Stellar activity GP model | ||
| h[m s−1] | 2.9 |
3.1 |
| λ [days] | 40.0 |
43.5 |
| w | 0.18 |
0.26 ± 0.07 |
| θ [days] | 40.4 |
39.8 |
| Uncorrelated jitter | ||
| σjit, HARPS-N [m s−1] | 1.4 ± 0.3 | 0.6 ± 0.4 |
| σjit, HARPS-pre [m s−1] | 2.2 ± 0.5 | 2.5 ± 0.5 |
| σjit, HARPS-post [m s−1] | 2.0 ± 0.6 | 1.6 ± 0.6 |
| RV offset | ||
| γHARPS-N [m s−1] | –0.06 |
30149.2 |
| γHARPS-pre [m s−1] | 0.20 |
30480.2 |
| γHARPS-post [m s−1] | 0.002 |
30479.2 ± 0.8 |
| Planetary orbital parameters | ||
| Kb [m s−1] | 2.7 ± 0.4 | 2.9 ± 0.4 |
| Pb [days] | 10.05454 ± 0.00003 | 10.05454 ± 0.00003 |
| T0,b [BJD-24 00 000] | 56813.42022 ± 0.00095 | 56813.42025 ± 0.00095 |
| Kc [m s−1] | 0.95 ± 0.37 | 0.98 ± 0.34 |
| Pc [days] | 24.64638 ± 0.00017 | 24.64638 ± 0.00018 |
| T0,c [BJD-24 00 000] | 56812.2777 ± 0.0026 | 56812.2778 ± 0.0026 |
| Kd [m s−1] | 0.29 [<0.43 (68.3th perc.)] |
0.31 [<0.47 (68.3th perc.)] |
| Pd [days] | 44.55764 ± 0.00042 | 44.55766 ± 0.00043 |
| T0,d [BJD-24 00 000] | 56826.2248 ± 0.0037 | 56826.2247 ± 0.0038 |
| Planetary radiia | ||
| Rp, b (R⊕) | 2.29 ± 0.23 | |
| Rp, c (R⊕) | 1.77 ± 0.18 | |
| Rp, d (R⊕) | 1.65 ± 0.17 | |
| Quantities derived from RVsb | ||
| Mp, b (M⊕) | 6.6 ± 1.1 | 7.0 ± 1.0 |
| Mp, c (M⊕) | 3.1 |
3.2 |
| Mp, d (M⊕) | 1.2 [<1.8 (68.3th perc.)] |
1.3 [<1.9 (68.3th perc.)] |
2.7 (see Sect. 5.1) |
||
| ρp, b [g cm−3] | 3.0 |
3.2 |
| ρp, c [g cm−3] | 3.1 |
3.2 |
| ρp, d [g cm−3] | 1.6 [<2.4 (68.3th perc.)] |
1.6 |
3.1 (see Sect. 5.1) |
||
| ap, b [AU] | 0.0777 |
|
| ap, c [AU] | 0.1413 |
|
| ap, d [AU] | 0.2097 |
|
Notes. Our global model includes three orbital equations (circular case). (a) Radii are derived using our estimate for the stellar radius, R = 0.60 ± 0.06 R⊙, and the ratios Rplanet∕Rstar derived by Beichman et al. (2016) from K2 and Spitzer data. (b)Derived quantities from the posterior distributions. We used the following equations (assuming Ms + mp≅Ms): mp sin i ≅ (
;
, where G is the gravitational constant.