Table 5
Orbital elements fitted on the astrometric data in Fig. 3.
| Parameter | A | B | |
|
|
|||
| Pb (yr) | 456.12 ± 2.81 | 456.12 ± 2.81 | |
| ib (°) | 18.50 ± 1.01 | 18.50 ± 1.01 | |
| Ωb (°) | 52.37 ± 10.31 | 52.37 ± 10.31 | |
| eb | – | – | |
| ωb (°) | – | – | |
| T0b (yr) | 1995.23 ± 13.88 | 1995.23 ± 13.88 | |
| ab (AU) | 67.98 ± 0.28 | 67.98 ± 0.28 | |
|
|
|||
| Pc (yr) | 228.06 ± 1.41 | 228.06 ± 1.41 | |
| ic (°) | 29.01 ± 0.47 | 29.01 ± 0.47 | |
| Ωc (°) | 61.83 ± 1.90 | 61.83 ± 1.90 | |
| ec | – | – | |
| ωc (°) | – | – | |
| T0c (yr) | 1845.87 ± 1.56 | 1845.87 ± 1.56 | |
| ac (AU) | 42.82 ± 0.18 | 42.82 ± 0.18 | |
|
|
|||
| Pd (yr) | 114.03 ± 0.70 | 114.03 ± 0.70 | |
| id (°) | 37.33 ± 0.48 | 37.33 ± 0.48 | |
| Ωd (°) | 57.94 ± 1.30 | 57.94 ± 1.30 | |
| ed | – | – | |
| ωd (°) | – | – | |
| T0d (yr) | 1965.68 ± 0.28 | 1965.68 ± 0.28 | |
| ad (AU) | 26.98 ± 0.11 | 26.98 ± 0.11 | |
|
|
|||
| Pe (yr) | 57.02 ± 0.35 | 46.24 ± 0.38 | |
| ie (°) | 31.16 ± 1.61 | 20.76 ± 4.85 | |
| Ωe (°) | 140.30 ± 8.60 | 82.52 ± 11.34 | |
| ee | – | – | |
| ωe (°) | – | – | |
| T0e (yr) | 1994.74 ± 1.16 | 1990.28 ± 1.47 | |
| ae (AU) | 16.99 ± 0.07 | 14.78 ± 0.08 | |
|
|
|||
|
1.15 | 1.15 | |
|
1.17 | 1.17 | |
|
1.45 | 1.45 | |
|
0.92 | 1.08 | |
|
|
|||
| M star (M⊙) | 1.51 | 1.51 | |
Notes. Case A: Orbital solution setting circular orbits and 8b:4c:2d:1e mean motion resonance. Case B: Orbital solution setting circular orbits and 4b:2c:1d and 5d:2e mean motion resonances. For each planet, the notations refer to the orbital period, inclination, longitude of the ascending node, eccentricity, argument of periapsis, time of periapsis passage, and semi-major axis. The error bars on the orbital parameters are at 1σ (see text). We also indicate the square root of the reduced χ2 for the nominal orbital solution for each planet and the mass assumed for the host star for the orbital fitting (see text). The semi-major axes are derived using Kepler’s third law assuming the fitted orbital periods and that the planet masses are negligible with respect to the mass of the star.
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