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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) [5012,80]
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) [0,0.3534]
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
RPR* Radius of planet in stellar radii
aR* 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)
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)
VcVe
e cos ω*
e sin ω*
MP sin i Minimum mass (ME) - 15.8 ± 1.6 14.4 ± 1.6
MPM* Mass ratio 0.0000594 ± 0.0000058 0.0000540 ± 0.0000058
dR* 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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