Table 2
Posterior stellar and planetary parameters obtained from our joint photometric and radial-velocity juliet analysis for TOI-269.
| Parameter name | Posterior estimate | Description |
|---|---|---|
| Posterior parameters for TOI-269 | ||
| ρ⋆ (g cm−3) |  |
Stellar density |
| q1,TESS |  |
Quadratic limb-darkening parameterization |
| q2,TESS |  |
Quadratic limb-darkening parameterization |
| q1,LCO |  |
Quadratic limb-darkening parameterization |
| q2,LCO |  |
Quadratic limb-darkening parameterization |
| q1,ExTrA |  |
Quadratic limb-darkening parameterization |
| q2,ExTrA |  |
Quadratic limb-darkening parameterization |
| Posterior parameters for TOI-269 b | ||
| Pb (days) |  |
Period of the planet |
| t0 (BJD TBD) |  |
Time of transit-center for the planet |
| r1,b |  |
Parameterization for p and b |
| r2,b |  |
Parameterization for p and b |
 |
 |
Parameterization for e and ω |
 |
 |
Parameterization for e and ω |
| Kb (m s−1) |  |
Radial-velocity semi-amplitude of the planet |
| Long-term trend in RVs | ||
| RV slope (m s−1 day−1) |  |
Linear trend : first parameter |
| RV intercept (km s−1) at tγ |  |
Linear trend: second parameter |
| Derived transit and RVs parameters | ||
| p = Rp∕R⋆ |  |
Planet-to-star radius ratio |
| b = (a∕R⋆) cos (ip) |  |
Impact parameter of the orbit |
| ip (deg) |  |
Inclination of the orbit |
| eb |  |
Eccentricity of the orbit |
| ωb (deg) |  |
Argument of periastron |
| Derived physical parameters(*) | ||
| Mp (M⊕) |  |
Planetary mass (in Earth mass) |
| Rp (R⊕) |  |
Planetary radius (in Earth radius) |
| ρp (g cm−3) |  |
Planetary density |
| ap (au) |  |
Semi-major axis |
| Teq (K) |  |
Equilibrium temperature of the planet(†) |
| S(S⊕) |  |
Planetary insolation (in Earth flux) |
Notes. The posterior estimate corresponds to the median value. Error bars denote the 68% posterior credibility intervals. (*) We sample from a normal distribution for the stellar mass, stellar radius, and stellar temperature that is based on the results from Sect. 2. (†) Equilibrium temperature was calculated assuming 0.3 Bond albedo and the semi-major axis distance.
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