Table 3
Best-fit values and priors of the model parameters for the combined RV+TESS photometry fit of TOI-179 discussed in Sect. 4.3.
| Parameter | Prior (a) | Best-fit value (b) | |
|---|---|---|---|
| RV linear trend (adopted) | RV parabolic trend | ||
| Fitted | |||
| RV stellar activity term | |||
| h (m s−1) | 𝒰(0,50) |  |
 |
| λ (days) | 𝒰(0,1000) |  |
 |
| ω | 𝒰(0,1) | 0.16 ± 0.03 | 0.16 ± 0.03 |
| θ (days) | 𝒰(3,10) | 8.72 ± 0.04 | 8.71 ± 0.04 |
| Planet-related parameters | |||
| Kb (m s−1) | 𝒰(0,50) |  |
 |
| orbital period, Pb (days) | 𝒰(4,4.2) |  |
4.1374355 ± 3.6 • 10−6 |
| Tconj,b [BJD-2450000] | 𝒰(9111.68,9111.78) |  |
 |
 |
𝒰(−1,1) |  |
 |
 |
𝒰(−1,1) |  |
 |
acceleration,  |
𝒰(0,0.1) | 0.048 ± 0.008 | 0.047 ± 0.011 |
curvature,  |
𝒰(−1,1) | – | 0.4 ± 2.2 • 10−5 |
| Rb/R⋆ | 𝒰(0.02,0.05) |  |
 |
| inclination, ib (deg) | 𝒰(80,90) |  |
 |
| RV-related parameters | |||
| σjit, HARPS−pre (ms−1 ) | 𝒰(0,20) |  |
 |
| γHARPS−pre (ms−1) | 𝒰(−100,+100) |  |
 |
| σjit, HARPS−post (m s−1 ) | 𝒰(0,20) |  |
 |
| γHARPS−post (m s−1) | 𝒰(−100,+100) |  |
 |
| Light curve-related parameters | |||
| σjit, TESS Sect. 2–3 | 𝒰(0,0.001) | 0 000177 ± 0 000009 | 0 000177 ± 0 000009 |
| σjit, TESS Sect. 29–30 | 𝒰(0,0.001) | 0.000185 ± 0.000009 | 0 000185 ± 0 000009 |
| LDc1 | 𝒰(0,1) |  |
 |
| LDc2 | 𝒰(0,1) |  |
 |
| Derived | |||
| ab (au) | – | 0.0480 ± 0.0004 | 0.0480 ± 0.0004 |
| eb | – |  |
 |
| ωb,⋆ (rad) | – |  |
−0.06 ±0.03 |
| ab/R⋆(c) | – |  |
 |
| impact param., b | – |  |
 |
| transit duration, T1,4 (days) | – |  |
 |
| radius, Rb (R⊕) | – |  |
 |
| mass, mb (M⊕) | – |  |
 |
| mean density, ρb (g cm−3) | – |  |
 |
| Surface gravity, ɡb (m s−2) | – | 35 ± 11 | 35 ± 11 |
| Log. Bayesian evidence, ln 𝒵 | 13971.5 | 13961.3 | |
Notes. (a)𝒰 denotes a prior drawn from an uninformative distributions. (b)Parameter uncertainties are given as the 16th and 84th percentiles of the posterior distributions. (c)We used the stellar density ρ*, [ρ⊙] as a free parameter with prior 𝒩(19,0.2), from which we derived ab/R⋆ at each step of the MC sampling. We recovered the prior distribution in the posterior of ρ*.
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