Table 4
Reference orbital parameters and their corresponding 99% credibility intervals.
| b | (h) | c | f | e* | ||
|
|
||||||
| P [days] | 7.2004 [7.1987, 7.2021] | 16.946 [16.872, 16.997] | 28.140 [28.075, 28.193] | 39.026 [38.815, 39.220] | 62.24 [61.69, 62.79] | |
| e | 0.13 [0.02, 0.23] | 0.06 [0, 0.38] | 0.02 [0, 0.17] | 0.03 [0, 0.19] | 0.02 [0, 0.24] | |
| K [m s-1] | 3.93 [3.55, 4.35] | 0.61 [0.12, 1.05] | 1.71 [1.24, 2.18] | 1.08 [0.62, 1.55] | 0.92 [0.50, 1.40] | |
| ω [rad] | 0.10 [5.63, 0.85] | 2.0 [0, 2π] | 5.1 [0, 2π] | 1.8 [0, 2π] | 0.5 [0, 2π] | |
| M0 [rad] | 3.42 [2.32, 4.60] | 5.1 [0, 2π] | 0.3 [0, 2π] | 5.1 [0, 2π] | 4.1 [0, 2π] | |
| λ [deg] | 201[168, 250] | 45(180)† | 308(99)† | 34 (170)† | 262(150)† | |
| Msini [M⊕] | 5.6 [4.3, 7.0] | 1.1 [0.2, 2.1] | 3.8 [2.6, 5.3] | 2.7 [1.5, 4.1] | 2.7 [1.3, 4.3] | |
| a [AU] | 0.0505 [0.0452, 0.0549] | 0.0893 [0.0800, 0.0977] | 0.125 [0.112, 0.137] | 0.156 [0.139, 0.170] | 0.213 [0.191, 0.232] | |
| d | g | Other model parameters | ||||
|
|
||||||
| P [days] | 91.61 [90.72, 92.42] | 256.2 [248.3, 270.0] | 
[m s-1 yr-1] |
2.07 [1.79, 2.33] | ||
| e | 0.03 [0, 0.23] | 0.08 [0, 0.49] | γHARPS [m s-1] | –30.6 [–34.8, –26.8] | ||
| K [m s-1] | 1.52 [1.09, 1.95] | 0.95 [0.51, 1.43] | γHIRES [m s-1] | –31.9 [–37.0, –26.9] | ||
| ω [rad] | 0.7 [0, 2π] | 0.9 [0, 2π] | γPFS [m s-1] | –25.8 [–28.9, –22.5] | ||
| M0 [rad] | 3.7 [0, 2π] | 4.1 [0, 2π] | σHARPS [m s-1] | 0.92 [0.63, 1.22] | ||
| σHIRES [m s-1] | 2.56 [0.93, 5.15] | |||||
| λ [deg] | 251(126)† | 285(170)† | σPFS [m s-1] | 1.31 [0.00, 3.85] | ||
| Msini [M⊕] | 5.1 [3.4, 6.9] | 4.6 [2.3, 7.2] | ||||
| a [AU] | 0.276 [0.246, 0.300] | 0.549 [0.491, 0.601] | ||||
Notes.While the angles ω and M0 are unconstrained due to strong degeneracies at small eccentricities, their sum λ = M0 + ω is better behaved and is also provided here for reference.
Values allowed in the full range of λ. Full-width-at-half-maximum of the marginalized posterior is provided to illustrate the most likely range (see Fig. 10).
Due to the presence of a strong alias, the orbital period of this candidate could be 53 days instead. Such an alternative orbital solution for planet e is given in Table B.2.
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