Table 5
All models fit to the joint Spitzer and K2 dataset.
| Parameter | Unit | Prior | (1)Toy model (F = 0) | Model name Toy model (F free) | Two temp. model |
|---|---|---|---|---|---|
| P | P-0.2803 d | u(1.690e–5, 3.190e–5) |  |
 |
 |
| t0 | BJDTDB - 2457744.0 d | u(0.07094, 0.07226) |  |
 |
 |
| Rp/R* | – | u(0.01807, 0.02267) |  |
 |
 |
| a/R* | – | N(2.36, 0.06) |  |
 |
 |
| cos i | – | u(0, 0.36975) |  |
 |
 |
| F | – | u(0, 0.5) | 0 (fixed) |  |
– |
| T* | K | N(4599, 79) |  |
 |
 |
| Tp,n | K | u(0, 4599) | – | – |  (<1712K 2σ, <2085 K 3σ) |
| Tp,d | K | u(0, 4599) | – | – |  |
| (<2635 2σ, <2857 K 3σ) | |||||
| Ag | – | u(0, 1) |  |
 |
 |
| ΔBIC | 0 | 12.0 | 22.2 |
Notes. The uniform priors on P, t0, Rp/R* cos i are based on the 5σ confidence interval of these parameters reported in Malavolta et al. (2018). The Gaussian prior for T* and a/R* are also from Malavolta et al. (2018). We derived the Gaussian prior for a/R* from the stellar density ρ* = (2.244 ± 0.161)ρo following a/R* ∝ (ρ*P2)1/3. N and u denote a Gaussian and uniform prior, respectively. (1)The Toy model without any redistribution (F = 0) provides the best fit to our data. We therefore recommend using the planetary parameters (P, t0, Rp/R*, a/R*, cos i) used in this column.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.