Table 2
Phase curve model parameters and priors used in the final joint analysis.
| Description | Parameter | Units | Prior | |||
|---|---|---|---|---|---|---|
| Global parameters | ||||||
| Mid-transit time | t0 | days | N(TS12)(a) | |||
| Orbital period | p | days | N(PS12)(a) | |||
| Area ratio | k2 | − | N(0.078, 0.005) | |||
| Stellar density | ρ | g cm−3 | N(0.54, 0.08) | |||
| Impact parameter | b | − | U(0, 1) | |||
 cos ω |
− | N4(0, 10−6) | ||||
 cos ω |
− | N(0, 10−6) | ||||
| EV offset | oEV | deg | N(0, 5) | |||
| Passband-dependent parameters | ||||||
| Quad. LD coeff. 1 | q1 | − | LDTK (b) | |||
| Quad. LD coeff. 2 | q2 | − | LDTK (b) | |||
| EV amplitude | AEV | − | U(c) | |||
| DB amplitude | ADB | − | U(d) | |||
| Emission offset | oe | deg | N(0, 10) | |||
| Log10 ds. emission | log10 fd | − | U(−3, 0) | |||
| Log10 ns. emission | log10 fn | − | U(−3, 0) | |||
| Geometric albedo | ag | − | N(10−5, 10−7) | |||
| Light-curve-dependent parameters | ||||||
| Baseline level | f0 | − | Ne | |||
| Log10 white noise | log10σ | − | N(f) | |||
| Ln GP input scale | si | − | N(1,1)(g) | |||
| Ln GP output scale | So | − | N(g) | |||
Notes. The global parameters are independent of passband or light curve, the passband-dependent parameters are repeated for each pass-band, and the light-curve-dependent parameters are repeated for each separate light curve. N(µ, σ) stands for a normal prior with a mean µ and standard deviation σ, and U(a, b) stands for a uniform distribution from a to b. (a)The zero epoch and orbital period priors are based on the values reported in Siverd et al. (2012) with uncertainties multiplied by three. (b)The limb darkening coefficients have normal priors calculated using LDTK. (c)Ellipsoidal variation is constrained based by EV amplitude ratios as explained in the text and listed in Table 3. (d)The Doppler beaming priors are given in Table 3. (e)The baseline levels have wide normal priors that are based on the light curve variability. (f)The average log white noise parameters have normal priors centred around a numerical white noise estimate. (g)The Gaussian process log input scales have wide normal priors while the log output scales have normal priors based on light curve variability.
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