Table 2
Results from the MCMC runs.
| Parameter | Prior | RV | Shadow | Slope |
|---|---|---|---|---|
| Stepping parameters | ||||
| P (days) | 𝒰 | 18.71205 ± 0.00001 | 18.71205 ± 0.00001 | 18.71205 ± 0.00001 |
| T0,b (BTJD) | 𝒰 | 1729.6814 ± 0.0004 | 1729.6814 ± 0.0004 | 1729.6814 ± 0.0004 |
| ΔT0,b(min.) | 𝒰 | 20 ± 3 | 18±3 | 22 ± 4 |
| r/R | 𝒰 | 0.0690 ± 0.0003 | 0.0689 ± 0.0003 | 0.0690 ± 0.0003 |
| a/R | 𝒰 |  |
 |
 |
| cos io | 𝒰 |  |
 |
 |
| λ (°) | 𝒰 | −1 ± 12 | −2±6 | 0±7 |
| v sin i (km s−1) | 𝒰 | 5.64 ± 0.14 | 5.63 ± 0.11 |  |
| ζ (km s−1) | 𝒩 (4.46,1.0) | 4.8 ± 0.4 | 4.7 ± 0.3 | 4.7 ± 0.2 |
| ξ (km s−1) | 𝒩 (2.0,1.0) |  |
 |
2.40 ± 0.17 |
| K (ms−1) | 𝒰 |  |
 |
17.5 ± 1.1 |
 |
𝒰 |  |
 |
 |
 |
𝒰 |  |
 |
 |
| γHARPS–N (ms−1) | 𝒰 | −23395.1 ± 1.1 |  |
−23344±12 |
| σHARPS-N (ms−1) | 𝒰 |  |
– | – |
| γLevy (ms−1) | 𝒰 | 1.0 ± 1.1 | 1.1 ± 1.1 |  |
| σLevy (ms−1) | 𝒰 |  |
 |
 |
| γHIRES (ms−1) | 𝒰 |  |
−1.6 ± 1.0 |  |
| σHIRES (ms−1) | 𝒰 |  |
 |
 |
| γSONG (ms−1) | 𝒰 | 2±6 |  |
2±6 |
| σSONG (ms−1) | 𝒰 | 18±5 |  |
 |
| q1 + q2 : TESS | 𝒩 (0.542,0.1) | 0.55 ± 0.03 | 0.56 ± 0.03 | 0.55 ± 0.03 |
| q1 + q2 : HARPS-N | 𝒩(0.7114,0.1) | 0.78 ± 0.08 | 0.78 ± 0.08 |  |
| log σSector 15 | 𝒰 |  |
−7.571 ± 0.008 | −7.571 ± 0.008 |
| log τsector 15 (log days) | 𝒰 |  |
 |
 |
| log ASector 15 | 𝒰 | −1.0 ± 0.3 | −1.0 ± 0.3 | −1.0 ± 0.3 |
| log σSector 14 | 𝒰 | −7.502 ± 0.008 | −7.502 ± 0.008 | −7.503 ± 0.008 |
| log τsector 14 (log days) | 𝒰 | −7.92 ± 0.04 | −7.91 ± 0.04 | −7.92 ± 0.04 |
| log ASector 14 | 𝒰 | −2.68 ± 0.11 |  |
 |
| log σSector 41 | 𝒰 | −8.127 ± 0.012 | −8.127 ± 0.012 |  |
| log τsector 41 (log days) | 𝒰 |  |
 |
 |
| log ASector 41 | 𝒰 |  |
 |
 |
| Derived parameters | ||||
| io (°) |  |
 |
 |
|
| b |  |
 |
 |
|
| e |  |
 |
 |
|
| ω(°) |  |
 |
 |
|
| r (RJupiter) | 0.857 ± 0 016 | 0.856 ± 0.016 | 0.857 ± 0.016 | |
| q1 : HARPS-N |  |
 |
 |
|
| q2 : HARPS-N |  |
 |
 |
|
| q1 : TESS |  |
 |
 |
|
| q2 : TESS |  |
 |
 |
|
Notes. Results from the MCMCs using the RVs, the planet shadow, and the local subplanetary velocity. The value is the median of the samples and the upper and lower uncertainties are estimated from the highest posterior density at a confidence level of 0.68. We denote the uniform priors as 𝒰 and the Gaussian priors with a mean, μ, and width, σ, as 𝒩(μ, σ). We chose the parameters obtained from analysing the deformation in the lines (the planetary shadow) as our final parameters. T0 is given in TESS Barycentric Julian Date (BTJD; BJD – 2 457 000).
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