Table 5
Best-fit posterior parameters and determined planet parameters for the two planetary systems.
| Parameter(a) | GJ 724 | GJ 3988 |
|---|---|---|
| Planetary posteriors | ||
| Pb (d) |  |
 |
| t0,b (BJD) |  |
 |
| Kb (m s−1) |  |
 |
 |
 |
0 (fixed) |
 |
 |
0 (fixed) |
| Derived parameters (b) | ||
| Mb sin i (M⊕) |  |
 |
| ab (au) |  |
 |
| eb |  |
0 (fixed) |
| ωb (deg) |  |
0 (fixed) |
| < Sb (S⊕)> |  |
 |
| < Teq,b (c) (K)> |  |
 |
| Teq,b (d) (K) |  |
 |
| GP posteriors | ||
| PGP,rv (d) |  |
 |
| σGP, rv, CARM-VIS (m s−1) |  |
 |
| σGP, rv, HARPS (m s−1) |  |
… |
| σGP,rv,IRD (m s−1) | … |  |
| ƒGP, rv |  |
 |
| Q0,GP, rv |  |
 |
| dQGP, rv |  |
 |
| Instrumental posteriors | ||
| γcarm-vis (m s−1) |  |
 |
| σCARM-VIS (m s−1) |  |
 |
| γHARPS (m s−1) |  |
… |
| σHARPS (m s−1) |  |
… |
| γIRD (m s−1) | … |  |
| σIRD (m s−1) | … |  |
Notes. (a) Error bars denote the 68% posterior credibility intervals.(b) These derived parameters were computed using the stellar parameters that were sampled from a normal distribution centred around the values from Table 1 with the width of the uncertainty.(c) Assuming a zero Bond albedo. (d) Computed using Eq. (4) from Quirrenbach (2022).
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