Table 2
Planetary parameters of the Kepler-278 and Kepler-391 systems.
| Parameter | Kepler-278b | Kepler-278c | Kepler-391b | Kepler-391c |
|---|---|---|---|---|
| Model parameters | ||||
| Kepler long-cadence additional white noise level | 2.495 ± 0.040 | 1.3993 ± 0.0095 | ||
| Kepler short-cadence additional white noise level | 1.1317 ± 0.0032 | N/A | ||
| Stellar mean density, ρ⋆ [g cm−3] (a) | 0.07237 ± 0.00096 | 0.0822  |
||
| Linear limb darkening, ua | 0.74  |
0.30  |
||
| Quadratic limb darkening, ub | −0.27  |
0.31  |
||
| Scaled semi-major axis, a∕R⋆ | 15.152 ± 0.067 | 21.541 ± 0.096 | 6.20  |
12.23  |
| Eccentricity, e (b) | 0.696  |
0.616  |
<0.46 (c) | <0.27 |
| Inclination, i [°] (d) | 85.11  |
88.58  |
85.5  |
87.27  |
| Argument of pericentre, ω [°] | 21.1 ± 7.7 | 20.80 ± 7.9 | 103  |
126  |
| Difference of the longitude of the ascending node, Ω1 − Ω2 [°] | 10  |
0 ± 74 | ||
 |
0.778  |
0.735  |
−0.06 ± 0.32 | −0.07  |
 |
0.295 ± 0.098 | 0.274 ± 0.093 | 0.35  |
0.16 ± 0.22 |
| Mean anomaly, M0 | 11.2  |
340.7 ± 1.7 | 321  |
227 ± 63 |
| Impact parameter, b | 0.544  |
0.27  |
0.38  |
0.561  |
| Epoch of transit, T0 [BJDTDB ] | 2 455 695.3727  |
2 455 700.4118 ± 0.0052 | 2 455 690.3959  |
2 455 696.9123  |
| Period, P [days] (e) | 30.1556  |
51.111  |
7.4175  |
20.501  |
| Radius ratio, Rp /R⋆ | 0.01266  |
0.01046 ± 0.00025 | 0.00795  |
0.00915 ± 0.00034 |
| Mass ratio, Mp /M⋆ | 0.000142  |
0.000087  |
<0.0026 | <0.0036 |
| Planet mean density, ρp [g cm−3 ] | 5.0  |
5.5  |
<380 | <400 |
| Derived properties | ||||
| Semi-major axis, a [AU] | 0.202 ± 0.005 | 0.287 ± 0.007 | 0.083  |
0.164  |
| Radius, Rp [R⊕ ] | 3.955 ± 0.080 | 3.268 ± 0.067 | 2.50 ± 0.29 | 2.88 ± 0.33 |
| Mass, Mp [M⊕ ] | 56  |
34.9  |
<1100 | < 450 |
| Incident flux, Sinc [S⊕ ] | 110 ± 14 | 54.3 ± 7.2 | 690  |
179  |
| Equilibrium temperature, Teq [K] (f) | 586 ± 19 | 492 ± 16 | 930  |
662  |
| Semiamplitude, K⋆ [m s −1 ] | 14.0  |
6.7  |
<340 | <93 |
Notes. (a) For Kepler-278 we used as prior the stellar density derived from asteroseismology by H13 and the one determined from stellar models in Sect. 3.3 for Kepler-391. (b)The orbital parameters correspond to Jacobi elements computed at the reference time tref = 2455695.37632 BJDTBD for Kepler-278 and at tref = 2455696.9123 BJDTBD for Kepler-391. (c) All upper limits correspond to the 95% confidence interval. (d)The prior for the inclination of planets b is uniform between [0, 180]°, and [0, 90]° for planets c. The value for the inclination in the table for planets b is reflected with respect to i = 90°, the supplementary angle is equally probable. (e)Defined as 
. (f) Calculated with Eq. (4) from Johnson et al. (2017) assuming a Bond albedo α of 0.3.
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