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![]() |
0.31![]() |
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![]() |
1.3![]() |
2.7![]() |
||
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![]() |
1.6![]() |
3.1![]() |
||
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.
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