Table 3
Derived planetary parameters of the HD 3167 system.
| Derived parameters | Symbols | Values | Units |
|---|---|---|---|
| Planet b | |||
| Optimal time of inferior conjunction |  |
 |
BJDTDB |
| Impact parameter | bb |  |
R* |
| Transit duration | T14, b |  |
h |
| Eccentricity(†) | eb (†) | < 0.10 (†) | |
| Semi-major axis | ab/R* |  |
– |
| ab | 0.01802 ± 0.00025 | AU | |
| Mass | Mb |  |
M⊕ |
| Radii | |||
| CHEOPS passband |  |
1.677 ± 0.036 | R⊕ |
| K2 passband |  |
 |
R⊕ |
| HST/WFC3/G141 passband |  |
 |
R⊕ |
| Spitzer/IRAC/Ch2 passband |  |
 |
R⊕ |
| All passbands | Rb |  |
R⊕ |
| Bulk densities | |||
| CHEOPS passband |  |
 |
g cm−3 |
| K2 passband |  |
 |
g cm−3 |
| HST/WFC3/G141 |  |
 |
g cm−3 |
| Spitzer/IRAC/Ch2 passband |  |
 |
g cm−3 |
| Equilibrium temperature(t) | Teq, b (‡) | 1777 ± 27(t) | K |
| Planet c | |||
| Optimal time of inferior conjunction |  |
 |
BJDTDB |
| Impact parameter | bc |  |
R* |
| Transit duration | T14, c |  |
h |
| Eccentricity(†) | ec (†) | < 0.15 (†) | – |
| Semi-major axis | ac/R* |  |
– |
| ac | 0.1783 ± 0.0025 | AU | |
| Mass | Mc |  |
M⊕ |
| Radii | |||
| K2 passband |  |
 |
R⊕ |
| HST/WFC3/G141 passband |  |
 |
R⊕ |
| Spitzer/IRAC/Ch2 passband |  |
 |
R⊕ |
| All passbands | Rc |  |
R⊕ |
| Bulk densities | |||
| K2 passband |  |
 |
g cm−3 |
| HST/WFC3/G141 |  |
 |
g cm−3 |
| Spitzer/IRAC/Ch2 passband |  |
 |
g cm−3 |
| Equilibrium temperature(‡) | Teq,c (‡) |  |
K |
| Planet d | |||
| Optimal time of inferior conjunction |  |
2457797.16 ± 0.21 | BJDTDB |
| Eccentricity(†) | ed (†) | <0.44(t) | – |
| Semi-major axis | ad/R* | 19.02 ± 0.23 | – |
| ad |  |
AU | |
| Minimum mass | Md sin id | 5.03 ± 0.50 | M⊕ |
| Equilibrium temperature(‡) | Teq,d (‡) |  (‡) |
K |
| Planet e | |||
| Eccentricity(†) | ee (†) | <0.60(†) | – |
| Semi-major axis | ae/R* |  |
– |
| ae |  |
AU | |
| Minimum mass | Me sin ie |  |
M⊕ |
| Equilibrium temperature(‡) | Teq,e (‡) |  |
K |
Notes. (†)Upper limits on the orbital eccentricities are computed with a confidence probability of 99.73%.(‡)Equilibrium temperatures are derived from the equation 
, which assumes black-body emissions for both the planet and the star, a Bond albedo AB = 0, and a perfect heat redistribution in the planetary atmosphere (uniform temperature).
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