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Table 2

Percentiles of the distributions in Fig. 2, referred to the cut for θ in the range 85–89 days, compared with values found by AE16.

Jump parameter Value
(This work) (Anglada-Escudé et al. 2016)

h [ m s-1] 1.91
λ [days] 311
w 0.34
θ [days] 87.1

γHARPSpre−2016 [ m s-1] 0.92 ± 0.56
γHARPSPRD [ m s-1] –0.58
γUVES [ m s-1] –0.48

K1 [ m s-1] 1.48 1.38 ± 0.21
P1 [days] 11.1855 11.186
Tc,1 [JD-2 400 000] 57 383.71
e1 0.17 <0.35
ω1 [rad] –2.49 5.41 (unconstrained)

dVr/ dt (·10-4) [ m s-1 day-1] 3.2 2.3 ± 8.4
σjit,HARPSpre−2016 [ m s-1] 1.11 ± 0.10 1.76
σjit,HARPSPRD [ m s-1] 0.63 1.14
σjit,UVES [ m s-1] 0.71 1.69

Minimum mass, mpsin i (M)a 1.21 ± 0.16 1.27
Orbital semi-major axis, a (AU)a 0.048 ± 0.002 0.0485

Notes. They represent our adopted solution for the one-planet model. Our analysis makes use of 13 parameters as well as three values γs for the offsets, while AE16 employed 26 parameters.

(a)

Derived quantities from the posterior distributions. We assumed Ms = 0.120 ± 0.015M as the mass of Proxima, and we used the following equations (assuming Ms + mpMs): mpsin i (; , where G is the gravitational constant.

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