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Table 3
Relative posterior probabilities and log-Bayesian evidences for different noise models using the HARPS RVs.
| Model | P(ℳ|d) | lnP(d|ℳ) |
|
|
||
| G | ~10-673 | −8431.0 |
| G+AR(1) | ~10-245 | −7446.0 |
| G+MA(1) | ~10-245 | −7447.3 |
| G+AR(3) | 3.2× 10-53 | −7004.5 |
| G+MA(3) | 1.1 × 10-48 | −6994.0 |
| G+MA(5) | 2.8 × 10-14 | −6914.8 |
| G+MA(7) | 1.9 × 10-9 | −6903.7 |
| G+MA(10) | 0.61 | −6884.1 |
| C+MA(10) | ~10-167 | −7267.1 |
| G+U+MA(10) | 0.39 | −6884.5 |
Notes. No Keplerian signals were included in the model. The noise models are Gaussian (G), Cauchy (C), Uniform (U), AR(q), and MA(p).
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