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Table 4

Results of the 1P+GP nested sampling modeling.

Parameter Unit Value
K (m s−1) 12517+16 $125_{-17}^{+16}$
P (d) 282748+61 $2827_{-48}^{+61}$
e 0.330.11+0.12 $0.33_{-0.11}^{+0.12}$
ω (deg) 31521+20 $315_{-21}^{+20}$
M0 (deg) 810+27 $8_{-10}^{+27}$
σjit (m s−1) 13.74.8+4.7 $13.7_{-4.8}^{+4.7}$
RVoff,Lick (m s−1) 4927+26 $-49_{-27}^{+26}$
RVoff,NIR (m s−1) 13332+32 $133_{-32}^{+32}$
RVoff,VIS (m s−1) 12432+32 $-124_{-32}^{+32}$
BGP ((m s−1)2) 29021015+1871 $2902_{-1015}^{+1871}$
PGP (d) 45938+72 $459_{-38}^{+72}$
LGP (d) 48434+433 $484_{-34}^{+433}$
CGP 0.040.04+0.74 $0.04_{-0.04}^{+0.74}$

ap (au) 4.400.13+0.19 $4.40_{-0.13}^{+0.19}$
mp sin (i) (MJup) 10.41.9+1.4 $10.4_{-1.9}^{+1.4}$
T0 (BJD) 2451510202+92 $2451510_{-202}^{+92}$

Notes. M0 represents the mean anomaly at the epoch of the first data point (BJD = 2451572.029297). T0 denotes the time of periastron passage and was derived from the best fit parameters. For each parameter, we give the mode of the posterior distribution. As uncertainties, we adopt the interval around the mode that encompasses 68% of the posterior samples. For the GP timescale LGP, due to the large plateau of low timescale solutions, the mode of the very asymmetric posterior is close to the prior boundary at 450 d. The GP hyperparameter CGP is poorly constrained. The full posteriors can be seen in Fig. D.1. ap and mp sin i were derived from the best parameters above. The uncertainties include the uncertainties of the stellar mass. If excluded, the uncertainties reduce to ap = 4.400.04+0.07 $4.40_{-0.04}^{+0.07}$ au and mp sin (i) = 10.41.7+1.3 $10.4_{-1.7}^{+1.3}$ MJup.

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