Table 4
Model and reference statistical parameters from the simultaneous fit of radial velocities and transit photometry.
| Parameter | One planet + GP(a) | Two planets | Two planets + GP | ||
|---|---|---|---|---|---|
| planet | b | b | c | b | c |
| P(d) | 4.052037 ± 0.000004 | 4.052039 ± 0.000005 | 16.04 ± 0.04 | 4.052037 ± 0.000005 | 16.06 |
| K(m s−1) | 17.6 ± 0.8 |  |
6.9 ± 0.3 | 17.4 |
6.3 |
| e | 0.04 ± 0.02 |  |
0.26 ± 0.06 | 0.04 ± 0.02 | 0.12 |
| ω (deg) | 219 ± 19 |  |
297 ± 112 | 21 ± 7 | 92 |
| tperi (d)(b) | 1.80 ± 0.23 |  |
7.3 ± 0.9 | 1.82 ± 0.09 | 14.0 |
| i(deg) | 87.3 ± 0.2 |  |
… | 87.3 ± 0.2 | … |
| Rp ∕R⋆ | 0.0751 ± 0.0009 |  |
… |  |
… |
| R⋆ (R⊙) | 0.57 ± 0.02 | 0.58 ± 0.02 | … | 0.57 ± 0.02 | … |
| u1 | 0.48 ± 0.08 | 0.5 ± 0.1 | … | 0.47 ± 0.10 | … |
| u2 (c) | 0.245 | 0.245 | … | 0.245 | … |
| Derived parameters | |||||
| a(au) | 0.0417 ± 0.0005 | 0.0417 ± 0.0005 | 0.104 ± 0.001 | 0.0417 ± 0.0005 | 0.104 ± 0.001 |
| λ (deg)(b,d) | 336.1 ± 0.8 | 337.0 ± 0.9 | 135 ± 12 | 336.8 |
134 ± 27 |
| tc (d)(b,e) | 0.38421 |
0.38401 |
13.22 |
0.38419 |
13.51 |
| mp (M⊕) | 30.8 ± 1.5 | 30.7 ± 0.8 | 18.4 ± 1.0 | 30.5 ± 1.2 | 17.2 |
| a∕R⋆ | 15.9 |
15.8 |
39.5 |
15.7 |
39.4 |
| Rp (R⊕) | 4.7 ± 0.3 | 4.8 ± 0.3 | … | 4.7 ± 0.3 | … |
| ρp (g cm−3) | 1.7 ± 0.3 |  |
… |  |
… |
| Teq (K)(f) | 700 |
703 |
444 |
706 |
445 |
| Instrumental parameters offset and weighted rms | |||||
| CARMENES VIS (m s−1 ] |  1.64 |
 4.28 |
 1.85 |
||
| CARMENES NIR (m s−1) |  12.3 |
 11.8 |
 12.3 |
||
| ESPRESSO (m s−1) |  0.50 |
 1.26 |
 0.52 |
||
| HIRES (m s−1) |  0.44 |
 2.80 |
 0.42 |
||
| PFS (m s−1) |  0.65 |
 2.49 |
 0.90 |
||
| iSHELL (m s−1) |  5.03 |
 7.61 |
 5.49 |
||
| GP hyper parameters | |||||
| Variance (m2 s−2) |  |
… |  |
||
| τd (d) |  |
… |  |
||
| − ln L | 316 | 336 | 303 | ||
| Red. χ2 | 0.81 | 2.64 | 1.04 | ||
Notes. Uncertainties are given as 68% intervals. The planetary parameters of the transiting planet from the different models are within 1-σ of each other, proving the consistency of this signal. Posterior distributions of the parameters are displayed in Fig. 11. The derived values for semi-major axis and planetary mass take the stellar mass uncertainty listed in Table 2 into account. The likelihood − ln L and the reduced χ2 is given for the RV fit. (a) We found the best model to be the one planet + GP model. (b)Reference time is BJD = 2458438. (c)Fixed. (d) Mean longitude. (e) Time of inferior conjunction. (f)Assuming zero albedo and full heat redistribution.
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