Table E.1
System parameters from Bayesian MCMC analysis.
| HD 27969 | HD 80869 | HD 95544 | HD 109286 | HD 115954 | HD 211403 | ||
|---|---|---|---|---|---|---|---|
| Planetary parameters | |||||||
| Mp sin ip [Mjup] |  |
 |
 |
 |
 |
 |
|
| Teq [K] |  |
 |
 |
 |
 |
 |
|
| P • [days] |  |
 |
 |
 |
 |
 |
|
 [BJD - 2 455 000] |
 |
 |
 |
 |
 |
 |
|
| tp [BJD - 2 455 000] |  |
 |
 |
 |
 |
 |
|
| a [AU]1 |  |
 |
 |
 |
 |
 |
|
| e |  |
 |
 |
 |
 |
 |
|
| ω* [°] |  |
 |
 |
 |
 |
 |
|
 |
 |
 |
 |
 |
 |
 |
|
 |
 |
 |
 |
 |
 |
 |
|
| a∕R* |  |
 |
 |
 |
 |
 |
|
| K • [m s−1] |  |
 |
 |
 |
 |
 |
|
| RV slope• [m s−1.y−1] |  |
 |
|||||
| Fi [Fi,⊕] |  |
 |
 |
 |
 |
 |
|
| Stellar parameters | |||||||
| RAGAIA-CRF2 [hh:mm:ss.ssss] | 4:26:49.6407 | 9:23:09.9103 | 11:05:17.5628 | 12:33:35.0020 | 13:19:56.4887 | 22:15:15.7963 | |
| DecGAIA-CRF2 [dd:mm:ss.ss] | 42:54:31.39 | 33:54:17.39 | 81:02:20.35 | 07:16:51.26 | 38:22:08.90 | 58:16:32.02 | |
| Sp. Type | G0V | G1V | G3V | G4V | G0V | F7V | |
| V mag | 7.65 | 8.45 | 8.39 | 8.77 | 8.34 | 8.50 | |
| M* [M⊙] | 1.16 ± 0.07 | 1.08 ± 0.05 | 1.09 ± 0.07 | 0.98 ± 0.05 | 1.18 ± 0.06 | 1.20 ± 0.06 | |
| R* R⊙] | 1.27 ± 0.10 | 1.062 ± 0.042 | 1.088 ± 0.072 | 1.089 ± 0.041 | 1.213 ± 0.083 | 1.206 ± 0.080 | |
| Teff [K] | 5966 ± 21 | 5837 ± 15 | 5722 ± 15 | 5694 ± 23 | 5957 ± 26 | 6273 ± 44 | |
| logg (dex) | 4.12 ± 0.04 | 4.18 ± 0.03 | 4.07 ± 0.03 | 4.44 ± 0.04 | 4.15 ± 0.04 | 4.30 ± 0.15 | |
| [Fe/H] [dex] | 0.18 ± 0.02 | 0.17 ± 0.01 | 0.11 ± 0.01 | 0.05 ± 0.02 | 0.34 ± 0.02 | 0.18 ± 0.04 | |
| v sin i* [km s−1] | 4.1 ± 1 | 3.7 ± 1 | 3.3 ± 1 | 3.8 ± 1 | 5.3 ± 1 | 18.4 ± 0.3 | |
| vturb [km s−1] | 1.17 ± 0.02 | 1.02 ± 0.02 | 1.02 ± 0.02 | 1.01 ± 0.03 | 1.15 ± 0.03 | ||
 [dex] |
−5.3 | −5.1 | −5.2 | −4.45 | −5.1 | −4.6 | |
 [km s−1 ] |
 |
 |
 |
 |
 |
 |
|
| Parameters of instruments | |||||||
 [m s−1 ] |
 |
 |
 |
||||
 [m s−1 ] |
 |
 |
 |
||||
 [m s−1 ] |
 |
 |
 |
 |
 |
 |
|
 [m s−1 ] |
< 11 | <6.8 |  |
||||
 [m s−1 ] |
 |
 |
 |
||||
Notes. –GAIA-CRF2 indicates that the coordinates are provided in the equatorial system with the Gaia Celestial Reference Frame (Gaia-CRF2 Gaia Collaboration 2018c).
– Spectral types are estimated from Teff using the Table 5 of Pecaut & Mamajek (2013).
– For M* and R* only statistical errors are included.
– The best-fit values are computed as the median of the cleaned MCMC chains.
– The errors bars correspond to 68% confidence intervals.
– The v sin i* values were obtained from the CCF using the SOPHIE pipeline (Boisse et al. 2010), except for the fast rotator HD 211403 for which the SME software was used (Valenti & Piskunov 1996). However, we not that for this star (Boisse et al. 2010) provides an estimate of 17.9 ± 1 km s−1 in good agreement with the SME value.
– The micro-turbulence velocity (vturb) is estimated as part of the spectroscopic stellar parameter derivation (Sect. 3.1). We refer the reader to Sousa (2014) for more details.
– The reference time for the RV slope model is the time of the first data point available in the data set.
–• indicates that the parameter is a main or jumping parameter for the MCMC explorations performed in Sect. 4.1.
–1Mp is inferred assuming an inclination of 
which is the average inclination assuming that the inclination are uniformly distributed in space (Lovis & Fischer 2010). a is computed from a∕R*.
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