Table 3
Properties of the KELT-9 planetary system.
| Stellar IDs | ||
|---|---|---|
| HD 195689 | ||
| TYC 3157-638-1 | ||
| 2MASS J20312634+3956196 | ||
| Stellar parameters | Source | |
| Star mass M⋆ [M⊙] | 2.32 ± 0.16 | This work |
| Star radius R⋆ [R⊙] | 2.418 ± 0.058 | This work |
| Stellar luminosity L⋆ [L⊙] |  |
This work |
| Stellar density ρ* [g cm−3] | 0.231 ± 0.025 | This work |
| Effective temperature Teff [K] | 9600 ± 400 | This work(a) |
| Derived effective temperature Teff [K] |  |
This work(b) |
| Surface gravity log g [cgs] | 4.1 ± 0.3 | This work(a) |
| Derived surface gravity log g [cgs] |  |
This work(b) |
| Metallicity [Fe∕H] [dex] | 0.14 ± 0.30 | This work(a) |
| Derived metallicity [Fe∕H] [dex] |  |
This work(b) |
| Age t [Gyr] |  |
This work |
| HARPS-N systemic velocity Vr, HN [km s−1] | − 19.819 ± 0.024 | This work |
| TRES radial-velocity zero point Vr, TRES [km s−1] | 0.391 ± 0.057 | This work |
| HARPS-N radial-velocity jitter sj,HN [km s−1] | 0.075 ± 0.048 | This work |
| TRES radial-velocity jitter sj,TRES [km s−1] | 0.138 ± 0.074 | This work |
| Gaia DR2 parallax π [mas] | 4.944 ± 0.050 | This work |
| Interstellar extinction AV |  |
This work |
| Stellar distance d [pc] | 202.3 ± 2.0 | This work |
| Transit and orbital parameters | Source | |
| Orbital period P [d] | 1.4811235 ± 0.0000011 | Gaudi et al. (2017) |
| Transit epoch T0[BJDTDB − 2 450 000] | 7095.68572 ± 0.00014 | Gaudi et al. (2017) |
| Radius ratio Rp∕R* | 0.08228 ± 0.00043 | Gaudi et al. (2017) |
| Inclination i [deg] | 86.79 ± 0.25 | Gaudi et al. (2017) |
| Orbital eccentricity e | 0 (fixed) | Gaudi et al. (2017) |
| Radial velocity semi-amplitude K [m s−1 ] | 293 ± 32 | This work |
| Planetary parameters | Source | |
| Planet mass Mp [MJup ] | 2.88 ± 0.35 | This work |
| Planet radius Rp [RJup ] | 1.936 ± 0.047 | This work |
| Planet density ρp [g cm−3 ] |  |
This work |
| Planet surface gravity log gp [cgs] |  |
This work |
| Orbital semi-major axis a [AU] | 0.03368 ± 0.00078 | This work |
| Equilibrium temperature Teq [K](c) |  |
This work |
Notes. (a) From the analysis of HARPS-N spectra. (b)From SED fitting and MIST evolutionary tracks by using the ExofastV2 tool and imposing Gaussian priors on Teff and [Fe∕H ] from the spectral analysis. (c)Black-body equilibrium temperature assuming a null Bond albedo and uniform heat redistribution to the night-side.
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