Table 1
Properties of the WASP-121 system.
| Parameter | Symbol | Value | Unit | Origin |
|---|---|---|---|---|
| Stellar properties | ||||
| Mass | M⋆ | 1.358 |
M⊙ | Delrez et al. (2016) |
| Radius | R⋆ | 1.458 ± 0.030 | R⊙ | Delrez et al. (2016) |
| Density | ρ⋆ | 0.434 ± 0.038 | ρ⊙ | Delrez et al. (2016)(†) |
| Limb-darkening coefficients | u1 | 0.364 |
EulerCam | |
| u2 | 0.146 |
EulerCam | ||
| Inclination |  |
8.1 |
deg | RM |
 |
171.9 |
deg | RM | |
| Equatorial velocity | veq | [65.28–120] | km s−1 | RM |
| Planetary properties | ||||
| Transit epoch | T0 | 2 458 119.72074 ± 0.00017 | BJDTDB | TESS |
| Orbital period | P | 1.27492504 |
d | (TESS+EulerCam) |
| Scaled semi-major axis | ap∕R⋆ | 3.8131 |
(TESS+EulerCam) | |
| Semi-major axis | ap | 0.02596 |
au | (TESS+EulerCam)(†) |
| Eccentricity | e | [0–0.0032] | TESS | |
| Argument of periastron | ω | 10 ± 10 | deg | TESS |
| Orbital inclination | ip | 88.49 ± 0.16 | deg | (TESS+RM) |
| Impact parameter | b | 0.10 ± 0.01 | (TESS+RM)(†) | |
| Transit durations | T14 | 2.9053 |
h | TESS(†) |
| T23 | 2.2605 |
h | TESS(†) | |
| Planet-to-star radius ratio |  |
0.12355 |
TESS | |
 |
0.12534 |
EulerCam | ||
| Radius |  |
1.753 ± 0.036 | RJup | TESS(†) |
 |
1.773 |
RJup | EulerCam(†) | |
| Stellar reflex velocity | K | 177.0 |
m s−1 | RV |
| Mass | Mp | 1.157 ± 0.070 | MJup | RV(†) |
| Density | ρp | 0.266 |
g cm−3 | (TESS+RV)(†) |
| Surface gravity | gp | 9.33 |
m s−2 | (TESS+RV)(†) |
| Sky-projected obliquity | λ | 87.20 |
deg | RM |
| 3D obliquity | ψNorth | 88.1 ± 0.25 | deg | RM(†) |
| ψSouth | 91.11 ± 0.20 | deg | RM(†) | |
Notes. Values in square brackets indicate the 1σ confidence intervals for the equatorial velocity and eccentricity, whose probability distributions peak at the lower boundary values for these parameters. The 3σ confidence intervals for these parameters are [65.28–295] km s−1 and [0–0.0078]. Properties with TESS origin are reported from Bourrier et al. (2019), or revised when combined with other datasets. Coefficients u1 and u2 are associated with a quadratic limb-darkening law. The daggers indicate derived parameters. Planetary density and surface gravity were calculated using the lowest planet-to-star radius ratio (from TESS). There are two possible solutions for the stellar inclination and 3D obliquity of WASP-121b, marked as North or South depending on which pole of the star is visible.
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