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Table 2
Planetary and stellar parameters to model the residual of the Rossiter–McLaughlin effect.
| Fitted parameters | |||
|---|---|---|---|
| Symbol (units) | Value | Prior | |
| Amplitude of planetary absorption | A (%) | −1.641 ± 0.063 | 𝒰(−2,−1) |
| Centre wavelength | λp (nm) | 850.042 ± 0.001 | 𝒰(850.03,850.05) |
| Slope of absorption | ∆λ | 0.523 ± 0.012 | 𝒰(0.475,0.575) |
| Gaussian width of absorption | σ (nm) | 0.029 ± 0.001 | 𝒰(0.02,0.04) |
| Planet-to-star radii ratio | Rp/R* | 0.074 ± 0.001 | 𝒰(0.069,0.076) |
| Projected spin-orbit angle | λ (deg) | 90.07 ± 0.24 | 𝒰(89,92) |
| Projected rotational velocity | υ sin i* (km s−1) | 95.05 ± 0.55 | 𝒰(90,105) |
| Fixed parameters | |||
| Symbol (units) | Value | Reference | |
| Orbital inclination | i (deg) |  |
Deline et al. (2022) |
| Scaled semi-major axis | a/R* |  |
Deline et al. (2022) |
| Limb-darkening parameters | u1 |  |
Deline et al. (2022) |
| u2 |  |
Deline et al. (2022) | |
Notes. Fitted and fixed parameters for the model in Eq. (12). All parameters except A, λp,vac, ∆λ, and σ were used to model the residual of the Rossiter–McLaughlin effect.
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