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Table D.1
Priors of the light curve fits
| Parameter | Prior | Dataset | Justification |
|---|---|---|---|
| Orbital model | |||
| ρ* [ρ⊙] | 𝒩(0.260,0.021) | All | From M* and R* derived in Section 3 |
| P [days] | 𝒩(1.80988198,6.0 10−7) | All | From Ehrenreich et al. (2020) |
| tic [TBJD] | 𝒩(2371.07202,8.3 10−4) | CHEOPS | Closest transit time to dataset centre, uncertainty propagated from ephemerides of Ehrenreich et al. (2020) except for IRAC1 and 2 for which we needed to enlarge the prior and chose an 8 min uncertainty. |
| 𝒩(2347.54356,8.2 10−4) | TESS | ||
| 𝒩 (1051.66806,8/24/60) | IRAC1 | ||
| 𝒩(859.82057,8/24/60) | IRAC2 | ||
| cos i | 𝒩(6.58 10−3,5.9 10−4) | All | From Ehrenreich et al. (2020) |
| e cos ω, e sin ω | ℐ(e : 𝒰(0,0.1),ω : 𝒰(−π,π)) | All | Joint prior: Priors are applied on e and ω computed from e cos ω, e sin ω. Upper boundary of e chosen to encompass upper limits by West et al. (2016) and Fu et al. (2021). |
| Transit model | |||
| Rp/R* | 𝒩(0.10852,0.10852 * 0.20) | All | Mean from Ehrenreich et al. (2020), uncertainty chosen to give margin for chromatic variations |
| u1 | 𝒩 (−0.0052,0.0118) | CHEOPS | |
| 𝒩 (0.0054,0.0145) | TESS | The priors were computed using the LDTK Python package (Parviainen & Aigrain 2015) which uses as input the Teff, logg, Fe/H derived by (Ehrenreich et al. 2020) | |
| 𝒩 (0.0569,0.0050) | IRAC1 | ||
| 𝒩 (0.0578,0.0084) | IRAC2 | ||
| u2 | 𝒩 (0.8660,0.0150) | CHEOPS | |
| 𝒩 (0.9486,0.0080) | TESS | ||
| 𝒩 (0.4825,0.0040) | IRAC1 | ||
| 𝒩 (0.3709,0.0090) | IRAC2 | ||
| u3 | 𝒩 (−0.0908,0.0076) | CHEOPS | |
| 𝒩 (−0.4383,0.0137) | TESS | ||
| 𝒩 (−0.4430,0.0029) | IRAC1 | ||
| 𝒩 (−0.3405,0.0038) | IRAC2 | ||
| u4 | 𝒩 (−0.1122,0.0025) | CHEOPS | |
| 𝒩 (0.0486,0.0088) | TESS | ||
| 𝒩 (0.1357,0.0020) | IRAC1 | ||
| 𝒩 (0.1061,0.0011) | IRAC2 | ||
| Occultation model when not part of a phase curve | |||
| Fp /F* [ppm] | 𝒰(0,5000) | IRAC1 | Upper limit chosen high enough not to impact the posterior |
| Phase curve model: Cos, Cos+Gauss or Gauss+Gauss | |||
| A0 [ppm] | 𝒰(0,1000) | CHEOPS | |
| 𝒰(0,1000) | TESS | Upper limit chosen high enough not to impact the posterior | |
| 𝒰(0,5000) | IRAC2 | ||
| σ0 [rad] | 𝒰(π/5,π/2) | CHEOPS | Boundaries chosen to separate the two components of the Gauss+Gauss model (see Appendix B.1) |
| 𝒰(0,1000) | CHEOPS | Upper limit chosen high enough not to impact the posterior | |
| Fn [ppm] | 𝒰(0,1000) | TESS | |
| 𝒰(0,5000) | IRAC2 | ||
| ϕ0 [rad] | 𝒰(−π/2,π/2) | All | Upper limit chosen high enough not to impact the posterior |
| A1 [ppm] | 𝒰(0,100) | CHEOPS+TESS | Upper limit chosen high enough not to impact the posterior |
| σ1 [rad] | 𝒰(0,π/6) | CHEOPS+TESS | Upper limit chosen to separate the two components of the Cos+Gauss and Gauss+Gauss models (see Appendix B.1) |
| ϕ1 [rad] | 𝒰(−π/2,π/2) | CHEOPS | Prior chosen broad enough not to impact the posterior |
| 𝒰(−π/4,π/4) | TESS | ||
| Phase curve model: Kelp,therm | |||
| C1,1 | 𝒰(0,1) | IRAC 1 & 2 | Priors recommended by Morris et al. (2022) |
| ƒ′ | 𝒰(0,1) | IRAC 1 & 2 | |
| ϕĸelp | 𝒰(−π/2,π/2) | IRAC 1 & 2 | Prior chosen broad enough not to impact the posterior |
| Phase curve model: Kelp,refl | |||
| Ag | ℐ(g:𝒰(−1, 1), ω0: 𝒰(0, 1), | CHEOPS, TESS | Joint prior: Used to put prior on g instead of Ag and ω0 + ω′ instead of ω′. The kelp function used to compute g tends to return NaN, so computing g and forcing finite and physical values to g help prevent execution errors. Regarding x1, x2, priors aim at probing reflective Eastern hemisphere due to produce flux excess before an eclipse. |
| ω0, ω′ | ω0 + ω′: 𝒰(0, 1), x1 : 𝒰(−π/2, −π/2 + π/8), | ||
| x1, x2 | x2: 𝒰(−π/8, π/2)) | ||
| Instrumental model | |||
| 𝒩(0.028, 0.001) | CHEOPS | ||
| c | 𝒩 (0.037,0.002) | TESS | See Sections 3 and 4.1. |
| 𝒩(0.095,0.005) | IRAC 1 | ||
| 𝒩 (0.090,0.004) | IRAC 2 | ||
| (ΔF/F)* |  |
All | Where med indicates the median, std the standard deviation, F is the measured flux and σc is the uncertainty on the contamination estimate. Where σF is the uncertainty on the measure flux. |
| σinst | 𝒰(0,5 · med(σF)) | All |
All the parameters in this table are introduced and described in Sections 4.1 and 4.2.
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