Table 2
Median values and 68% confidence interval for HD 207897 b and its host star.
Parameter | Units | Model priors | Activity on 35.9 d (Prob. = 46%) | Activity on 37.6 d (Prob. = 54%) | ||
---|---|---|---|---|---|---|
Stellar parameters: | ||||||
M* | Mass (M⊙) | – | ![]() |
![]() |
||
R* | Radius (R⊙) | – | ![]() |
![]() |
||
R*,SED | Radius(1) (R⊙) | – | ![]() |
![]() |
||
L* | Luminosity (l⊙) | – | ![]() |
![]() |
||
FBol | Bolometric Flux (cgs) | – | ![]() |
![]() |
||
ρ* | Density (cgs) | – | ![]() |
![]() |
||
logg | Surface gravity (cgs) | – | ![]() |
![]() |
||
Teff | Effective Temperature (K) | ![]() |
![]() |
![]() |
||
Teff,SED | Effective Temperature(1) (K) | – | ![]() |
![]() |
||
[Fe/H] | Metallicity (dex) | ![]() |
![]() |
![]() |
||
![]() |
Initial Metallicity(2) | – | ![]() |
![]() |
||
Age | Age (Gyr) | – | ![]() |
7.1 ± 4.5 | ||
EEP | Equal Evolutionary Phase(3) | – | ![]() |
![]() |
||
AV | V-band extinction (mag) | ![]() |
![]() |
![]() |
||
σSED | SED photometry error scaling | – | ![]() |
![]() |
||
ϖ | Parallax (mas) | ![]() |
![]() |
35.345 ± 0.047 | ||
d | Distance (pc) | – | 28.292 ± 0.038 | 28.293 ± 0.038 | ||
![]() |
RV slope(4) (m s−1/day) | – | − 0.00078 ± 0.00030 | ![]() |
||
Planetary parameters: | ||||||
P | Period (days) | – | 16.202157 ± 0.000085 | ![]() |
||
RP | Radius (RE) | – | ![]() |
![]() |
||
MP | Mass (ME) | – | 15.9 ± 1.6 | 14.4 ± 1.6 | ||
TC | Time of conjunction(5) (BJDTDB) | – | ![]() |
![]() |
||
TT | Time of minimum projected separation(6) (BJDTDB) | – | ![]() |
![]() |
||
T0 | Optimal conjunction Time(7) (BJDTDB) | – | ![]() |
![]() |
||
a | Semi-major axis (AU) | – | ![]() |
![]() |
||
i | Inclination (Degrees) | – | ![]() |
88.757 ± 0.067 | ||
e | Eccentricity | – | ![]() |
![]() |
||
ω* | Argument of Periastron (Degrees) | – | ![]() |
− 100 ± 110 | ||
Teq | Equilibrium temperature(8) (K) | – | ![]() |
![]() |
||
τcirc | Tidal circularization timescale (Gyr) | – | ![]() |
![]() |
||
K | RV semi-amplitude (m s−1) | – | 4.65![]() |
4.24![]() |
||
RP∕R* | Radius of planet in stellar radii | – | ![]() |
![]() |
||
a∕R* | Semi-major axis in stellar radii | – | ![]() |
![]() |
||
δ | Transit depth (fraction) | – | ![]() |
![]() |
||
Depth | Flux decrement at mid transit | – | ![]() |
![]() |
||
τ | Ingress/egress transit duration (days) | – | ![]() |
![]() |
||
T14 | Total transit duration (days) | – | ![]() |
![]() |
||
TFWHM | FWHM transit duration (days) | – | ![]() |
![]() |
||
b | Transit Impact parameter | – | ![]() |
![]() |
||
bS | Eclipse impact parameter | – | ![]() |
![]() |
||
τS | Ingress/egress eclipse duration (days) | – | ![]() |
![]() |
||
TS,14 | Total eclipse duration (days) | – | ![]() |
![]() |
||
TS,FWHM | FWHM eclipse duration (days) | – | 0.1143 ± 0.0015 | 0.1143 ± 0.0016 | ||
δS,2.5μm | Blackbody eclipse depth at 2.5μm (ppm) | – | ![]() |
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||
δS,5.0μm | Blackbody eclipse depth at 5.0μm (ppm) | – | ![]() |
![]() |
||
δS,7.5μm | Blackbody eclipse depth at 7.5μm (ppm) | – | ![]() |
![]() |
||
ρP 3 | Density (cgs) | – | 5.52![]() |
5.05![]() |
||
log gP | Surface gravity | – | 3.393![]() |
3.353![]() |
||
Θ | Safronov Number | – | 0.0647![]() |
0.0589![]() |
||
⟨F⟩ | Incident Flux (109 erg s−1 cm−2) | – | ![]() |
![]() |
||
TP | Time of Periastron (BJDTDB) | – | ![]() |
![]() |
||
TS | Time of eclipse (BJDTDB) | – | ![]() |
![]() |
||
TA | Time of Ascending Node (BJDTDB) | – | ![]() |
![]() |
||
TD | Time of Descending Node (BJDTDB) | – | ![]() |
![]() |
||
Vc ∕Ve | – | ![]() |
![]() |
|||
e cos ω* | – | ![]() |
![]() |
|||
e sin ω* | – | ![]() |
![]() |
|||
MP sin i | Minimum mass (ME) | - | 15.8 ± 1.6 | 14.4 ± 1.6 | ||
MP ∕M* | Mass ratio | – | 0.0000594 ± 0.0000058 | 0.0000540 ± 0.0000058 | ||
d∕R* | Separation at mid transit | – | ![]() |
![]() |
||
PT | A priori non-grazing transit prob | - | ![]() |
![]() |
||
PT,G | A priori transit prob | – | ![]() |
![]() |
||
PS | A priori non-grazing eclipse prob | – | ![]() |
![]() |
||
PS,G | A priori eclipse prob | – | ![]() |
![]() |
||
Stellar activity parameters: | ||||||
PActivity | Period (days) | – | 35.923![]() |
37.627![]() |
||
TC,activity | Time of conjunction(5) (BJDTDB) | – | 2458917.1 ± 2.2 | 2458910.7![]() |
||
eActivity | Eccentricity | – | ![]() |
![]() |
||
ω*, activity | Argument of Periastron (Degrees) | – | -127![]() |
33![]() |
||
KActivity | RV semi-amplitude (m s−1) | – | ![]() |
![]() |
||
Telescope parameters for SOPHIE: | ||||||
γrel | Relative RV Offset(4) (m s−1) | – | − 6327.36 ± 0.56 | − 6327.53 ± 0.52 | ||
σJ | RV Jitter (m s−1) | – | ![]() |
![]() |
||
![]() |
RV Jitter Variance | – | ![]() |
![]() |
||
Telescope parameters for APF: | ||||||
γrel | Relative RV Offset(4) (m s−1) | – | 3.1 ± 1.1 | ![]() |
||
σJ | RV Jitter (m s−1) | – | ![]() |
![]() |
||
![]() |
RV Jitter Variance | – | ![]() |
![]() |
||
Telescope parameters for HIRES: | ||||||
γrel | Relative RV Offset(4) (m s−1) | – | ![]() |
![]() |
||
σJ | RV Jitter (m s−1) | – | 2.15![]() |
2.42![]() |
||
![]() |
RV Jitter Variance | – | ![]() |
![]() |
||
Wavelength parameters: | TESS | TESS | ||||
u1 | linear limb-darkening coeff | – | 0.386 ± 0.046 | ![]() |
||
u2 | quadratic limb-darkening coeff | – | 0.188 ± 0.048 | ![]() |
||
Transit prameters: | TESS UT 2019-10-10 (TESS) | TESS UT 2019-10-10 (TESS) | ||||
σ2 | Added Variance | – | 0.0000000244 ± 0.0000000011 | 0.0000000244 ± 0.0000000011 | ||
F0 | Baseline flux | – | ![]() |
![]() |
Notes. Gaussian priors are presented by
where a and b are the mean and width, respectively. Likewise, the uniform prior is denoted by
and c and d present bounds on the parameter. The two solutions correspond to two possibilities for the stellar activity period. The highlighted parameters present a difference exceeding 0.5 σ between thetwo solutions. See Table 3 in Eastman et al. (2019) for a detailed description of all parameters. (1) This value ignores the systematic error and is for reference only. (2)The metallicity of the star at birth. (3)Corresponds to static points in a star’s evolutionary history. See Sect. 2 in Dotter (2016). (4) Reference epoch = 2456438.359500. (5) Time of conjunction is commonly reported as the “transit time”. (6)Time of minimum projected separation is a more correct “transit time”. (7) Optimal time of conjunction minimizes the covariance between TC and Period. (8)Assumes no albedo and perfect redistribution.
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