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Table 2
Modeled and inferred parameters for GJ 163 system.
| Unit | Prior | Posterior | |
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| Systemic velocity, γ | [km s-1] | Uniform (γmin = −100, γmax = + 100) | 58.59728 ± 0.00026 |
| Orbital period, Pb | [days] | Jeffreys (Pmin = 1, Pmax = 104) | 8.63182 ± 0.00155 |
| Radial-velocity semi-amplitude, Kb | [m/s] | Jeffreys (Kmin = 0.1, Kmax = 100) | 6.13 ± 0.33 |
| Orbital eccentricity, eb | [ ] | Uniform (emin = 0, emax = 0.91) | 0.073 ± 0.050; <0.101 (1-σ upper limit) |
| Argument of periastron, ωb | [rad] | Uniform (ωmin = 0, ωmax = 2π) | 1.234 ± 0.953 |
| Mean longitude, λb | [rad] | 0.111 ± 0.274 | |
| Semi-major axis, ab | [AU] | 0.06070 ± 0.00001 | |
| Time of inferior conjunction, Ttr,b | [days] | 52 936.1209 ± 0.4038 | |
| Planetary minimum mass, mbsini | [M⊕] | 10.6 ± 0.6 | |
| Orbital period, Pc | [days] | Jeffreys (Pmin = 1, Pmax = 104) | 25.63058 ± 0.02550 |
| Radial-velocity semi-amplitude, Kc | [m/s] | Jeffreys (Kmin = 0.1, Kmax = 100) | 2.75 ± 0.35 |
| Orbital eccentricity, ec | [ ] | Uniform (emin = 0, emax = 0.91) | 0.099 ± 0.086; <0.144 (1-σ upper limit) |
| Argument of periastron, ωc | [rad] | Uniform (ωmin = 0, ωmax = 2π) | 3.962 ± 1.394 |
| Mean longitude, λc | [rad] | 0.428 ± 0.524 | |
| Semi-major axis, ac | [AU] | 0.1254 ± 0.0001 | |
| Time of inferior conjunction, Ttr,c | [day] | 52 922.2303 ± 2.2951 | |
| Planetary minimum mass, mcsini | [M⊕] | 6.8 ± 0.9 | |
| Orbital period, Pd | [days] | Jeffreys (Pmin = 1, Pmax = 104) | 603.95116 ± 7.55862 |
| Radial-velocity semi-amplitude, Kd | [m/s] | Jeffreys (Kmin = 0.1,Kmax = 100) | 4.42 ± 0.51 |
| Orbital eccentricity, ed | [ ] | Uniform (emin = 0, emax = 0.91) | 0.373 ± 0.077 |
| Argument of periastron, ωd | [rad] | Uniform (ωmin = 0, ωmax = 2π) | 2.064 ± 0.357 |
| Mean longitude, λd | [rad] | 2.530 ± 0.301 | |
| Semi-major axis, ad | [AU] | 1.0304 ± 0.0086 | |
| Time of inferior conjunction, Ttr,d | [days] | 52 876.6622 ± 35.8448 | |
| Planetary minimum mass, mdsini | [M⊕] | 29.4 ± 2.9 | |
Notes. Tepoch = 52 942.80392 days. An additional 10% uncertainty should be added quadratically to the planetary mass uncertainties when accounting for the 10% uncertainty on the stellar mass.
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