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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 RplanetRstar 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 + mpMs): mp sin i ≅ (; , where G is the gravitational constant.

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