Table 4
Priors and derived posteriors for the parameters used in the spectral retrieval analyses.
| Parameter | Prior | Posterior | |||||
|---|---|---|---|---|---|---|---|
| Model A.i | Model B.i | Model C.i | Model D.ii | Model E.i | Model F.i | ||
| Tiso (K) | 𝒰(500, 1500) | – | ![]() |
![]() |
– | ![]() |
![]() |
| log P0 (log bar) | 𝒰(−6, 2) | – | ![]() |
![]() |
– | ![]() |
![]() |
| log Pcloud (log bar) | 𝒰(−6, 2) | – | ![]() |
![]() |
– | ![]() |
![]() |
| log ARS | 𝒰(−4, 4) | – | ![]() |
![]() |
– | ![]() |
![]() |
| ϕ | 𝒰(0, 1) | – | ![]() |
![]() |
– | ![]() |
![]() |
| Rp (RJup) a | 𝒰(−0.5, 1.5) | ![]() |
– | – | ![]() |
– | – |
| Tphot (K) | 𝒩(4987, 41) | – | – | – | ![]() |
![]() |
![]() |
(K) |
𝒰(−2500, 2500) | – | – | – | ![]() |
![]() |
![]() |
![]() |
𝒰(0, 1) | – | – | – | ![]() |
![]() |
![]() |
(K) |
𝒰(−2500, 2500) | – | – | – | ![]() |
![]() |
![]() |
![]() |
𝒰(0, 1) | – | – | – | ![]() |
![]() |
![]() |
| C/O | 𝒰(0.1, 1.6) | – | ![]() |
– | – | ![]() |
– |
| log Z (Z⊙) | 𝒰(−2, 3) | – | ![]() |
– | – | ![]() |
– |
| log XNa | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
| log XK | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
| log XTiO | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
| log XVO | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
| log XCO | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
| log XHCN | 𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
![]() |
𝒰(−12, 0) | – | – | ![]() |
– | – | ![]() |
| log XSiO | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
| log XFeH | 𝒰(−12, 0) | – | – | ![]() |
– | –![]() |
|
| ∆offset (ppm) | 𝒰(−5000, 5000) | ![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
Notes. (a)In the flat-line and pure stellar contamination models, the baseline transit depth was parameterized in terms of the planetary radius, Rp. For models incorporating atmospheric assumptions, the transit depth was directly fit based on the atmospheric parameters, and Rp was omitted from the parameter set.
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