Table 2
Best-fit and derived parameters from the RV analysis.
| Parameter | Value | Units | Assumptionsa |
|
|
|||
| K | 93 ± 17 | m/s | e (REB), P (TR) |
| V sys | −62.011 ± 0.011 | km s-1 | e (REB), P (TR) |
| ω | 250 ± 100 | deg. | e (REB), P (TR) |
| Mpsini | 1.01 ± 0.18 | M Jup | e (REB), P (TR), M⋆ (AS) |
| a | 0.0726 ± 0.0019 | AU | e (REB), P (TR), M⋆ (AS) |
|
|
|||
| M p | 1.09 ± 0.20 | M Jup | i (TR) |
| ρ p |
|
ρ Jup | Rp (TR) |
| a / R ⋆ | 2.48 ± 0.12 | R⋆ (AS) | |
Notes. Parameters below the horizontal line are derived from those above.
Assumed parameters and the method used to determine them. Parameters: e (eccentricity), P (period), M⋆ (stellar mass), i (orbital inclination), Rp (planet radius), and R⋆ (stellar radius). Methods: AS = asteroseismology , TR = transit fitting , REB = light-curve modulations fitting. Assumed values are taken from Lillo-Box et al. (2014b).
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