Table 3
Best-fit results of the π Men photometry+RV joint modelling.
| Jump parameter | Prior | Best-fit value | Literature | ||
|---|---|---|---|---|---|
| π Men c: circular (adopted) | π Men c: eccentric | ||||
| Kb [m s−1] |  (185.6,199.6) |
196.1 ± 0.7 | 196.0 |
195.8 ± 1.4 (a); 192.6 ± 1.4 (b) | |
| Pb [days] |  (2084.42, 2101.72) |
2088.8 ± 0.4 | 2088.8 ± 0.4 | 2091.2 ± 2.0 (a); 2093.07 ± 1.73 (b) | |
| Tb, conj [BJD-2 450 000] |  (8590.2, 8674.2) |
8632.6 ± 1.1 | 8632.7 ± 1.2 | 6548.2 ± 2.7 (a); −3913.0 ± 8.4 (b) | |
| eb cos ω⋆, b |  (−1, 1) |
0.5552 ± 0.0014 | 0.5551 |
– | |
| eb sin ω⋆, b |  (−1, 1) |
−0.3220 |
−0.3221 |
– | |
| Kc [m s−1] |  (0,5) |
1.5 ± 0.2 | 1.5 |
1.55 ± 0.27 (a); 1.58 (b) |
|
| Pc [days] |  (6.2679,0.00046) |
6.267852 ± 0.000016 | 6.267852 |
6.26834 ± 0.00024 (a); 6.2679 ± 0.00046 (b) | |
| Tc, conj [BJD-2 450 000] |  (8519.8066,0.0012) |
8519.8068 ± 0.0003 | 8519.8065 |
8325.503055 ± 0.00077 (a); 8325.50400 (b) |
|
| ec cos ω⋆, c |  (−1, 1) (c) |
0 (fixed) | −0.03 ± 0.06 | 0 (a),(b) | |
| ec sin ω⋆, c |  (−1, 1) (c) |
0 (fixed) | −0.11 |
0 (a),(b) | |
| σjit, UCLES [m s−1] |  (0,50) |
4.1 |
4.0 |
4.26 (a); 6.7 ± 0.60 (b) |
|
| σjit, CORALIE-98 [m s−1] |  (0,50) |
4.3 |
4.3 ± 0.1 | – | |
| σjit, CORALIE-07 [m s−1] |  (0,50) |
13.3 |
13.7 |
– | |
| σjit, CORALIE-14 [m s−1] |  (0,50) |
13.2 |
13.4 |
– | |
 [m s−1] |
 (0,10) |
2.3 ± 0.3 | 2.3 ± 0.3 | 2.35 (a); 2.33 ± 0.18 (b) |
|
 [m s−1] |
 (0,10) |
1.8 |
1.8 |
1.69 (a); 1.74 ± 0.33 (b) |
|
 [m s−1] |
 (0,10) |
1.2 |
1.2 |
– | |
 [m s−1] |
 (0,10) |
1.2 ± 0.2 | 1.3 ± 0.3 | – | |
| γCORALIE-98 [m s−1] |  (10600,10800) (d) |
10 674.0 |
10 674.6 ± 5.0 | – | |
| γCORALIE-07 [m s−1] |  (−100,+100) (e) |
−3.2 |
−3.6 |
– | |
| γCORALIE-14 [m s−1] |  (0,200) (e) |
21.9 |
21.5 ± 5.0 | – | |
 [m s−1] |
 (10600,10800) (d) |
10 707.0 ± 1.0 | 10 707.0 ± 1.1 | – | |
 [m s−1] |
 (−10,+40) (e) |
22.7 ± 0.8 | 22.7 ± 0.8 | – | |
 [m s−1] |
 (10600,10800) (d) |
10 639.0 ± 2.0 | 10 639.1 ± 2.0 | – | |
 [m s−1] |
 (−30,+10) (e) |
−1.3 ± 2.0 | −1.3 ± 2.0 | – | |
| Rc ∕R* |  (0,0.1) |
0.0165 ± 0.0001 | 0.0166 ± 0.0004 | 0.01721 ± 0.00024 (a); 0.01703 (b) |
|
| ac ∕R* | (f) | 12.5 ± 0.3 | 11.2 ± 1.9 | 13.10 ± 0.18 (a); 13.38 ± 0.26 (b) | |
| ic [deg] |  (0,90) (g) |
87.05 ± 0.15 | 86.9 |
87.31 ± 0.11 (a); 87.456 (b) |
|
| σjit, TESS [ppm] |  (0,300) |
130 ± 2 | 130 ± 2 | – | |
| limb darkening coeff q1 |  (0.280,0.002) |
0.280 ± 0.002 | 0.280 ± 0.002 | ||
| limb darkening coeff q2 |  (0.270,0.002) |
0.270 ± 0.002 | 0.270 ± 0.002 | ||
| Derived planetary parameters | |||||
| Eccentricity, eb | 0.642 ± 0.001 | 0.642 ± 0.001 | 0.6394 ± 0.0025 (a); 0.637 ± 0.002 (b) | ||
| Argument of periastron, ω⋆, b [deg] | − 30.1 ± 0.3 | −30.1 ± 0.3 | −29.3 ± 0.7 (a); −29.4 ± 0.3 (b) | ||
| Tb, periastron [BJD-2 450 000] | 8388.6 ± 2.2 | 8387.4 ± 2.2 | |||
| Minimum mass, mb sin ib [MJup ] | 9.89 ± 0.25 | 9.89 ± 0.25 | 9.66 ± 0.20 (a); 10.02 ± 0.15 (b) | ||
| Orbital semi-major axis, ab [au] | 3.28 ± 0.04 | 3.28 ± 0.04 | 3.22 ± 0.03 (a); 3.10 ± 0.02 (b) | ||
| Eccentricity, ec | 0 (fixed) | 0.15 (<0.21 68%) |
0 (a),(b) | ||
| Argument of periastron, ω⋆, c [deg] | 90 (fixed) | −93.7 |
0 (a),(b) | ||
| Orbital semi-major axis, ac [au] | 0.0680 ± 0.0008 | 0.0680 ± 0.0009 | 0.06702 ± 0.00109 (a); 0.06839 ± 0.00050 (b) | ||
| Mass, mc [M⊕ ] | 4.3 ± 0.7 | 4.5 ± 0.7 | 4.52 ± 0.81 (a); 4.82 (b) |
||
| Radius, Rc [R⊕ ] | 2.11 ± 0.05 | 2.11 ± 0.07 | 2.06 ± 0.03 (a); 2.04 ± 0.05 (b) | ||
| Average density, ρc [g cm−3 ] | 2.8 ± 0.5 | 2.8 ± 0.5 | 2.82 ± 0.53 (a); 2.97 (b) |
||
| ΔBIC | 0 | +19 | |||
| RMS of the RV residuals [ m s−1 ] | All data | 5.6 | |||
| HARPS | 2.2 | ||||
| ESPRESSO | 1.2 | ||||
Notes. Values are given as the 50th percentile of the posterior distributions, and the uncertainties are derived from the 16th and 84th percentiles. (a) After Gandolfi et al. (2018). (b) After Huang et al. (2018). (c) The eccentricity was further constrained to values < 0.75. (d).Relative to the UCLES dataset, which is used as reference. (e) Relative to the “pre” dataset of the corresponding instrument. (f) In the analysis we used the stellar density ρ* [ρ⊙ ] as a free parameter (
(0.67,0.04)), from which we derived ac∕R* at each step of the Monte Carlosampling. (g)We used cos ic
as a free parameter.
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