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Table E.1
Prior and posterior distributions for our first run de- signedto converge to the best region of the parameter space quickly (
- Uniform; 
- Gaussian; 
- Jeffreys; 
- beta distribution).
| Parameter | Prior | Posterior(a) |
|---|---|---|
| Stellar density ρ* [g.cm−3] |  [0.2590, 0.0150] |
 [0.257, 0.02] |
| HD 137496 b | ||
| Period Pb [days] |  [1.621, 0.0005] |
 [1.6211, 0.0001] |
| RV semi-amplitude Kb [m s−1] |  [0.0, 50.0] |
 [2.14, 0.3] |
| Radius ratio Rp,b∕R* |  [0.0, 1.0] |
 [0.0076, 0.0003] |
| Time of inferior conjunction tic,b [BJD-2450000] | ϕ :  (b) |
 [58039.132, 0.003] |
| Cos inclination cosib [°] | - |  [0.072, 0.06] |
| HD 137496 c | ||
| Period Pc [days] |  [0.1, 740] |
 [481.6, 3.0] |
| RV semi-amplitude Kc [m s−1] |  [230, 100] |
 [221.26, 0.9] |
| Time of inferior conjunction tic,c [BJD-2450000] | ϕ :  (b) |
 [58629.22, 0.5] |
Notes. (a)Starting distribution from which the samples were drawn for the first step in our MCMC analysis. (b)As defined in Table 4.
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