Table 4
Maximum a posteriori (MAP) estimation of the parameters for the noise model (lower rows) and the five signals (upper rows) detected in the TERRA-reduced HARPS data for HD 20794.
| Parameters | HD 20794 b | HD 20794 d | HD 20794 e | HD 20794 f? | HD 20794 g? | HD 20794 c? |
|
|
||||||
| P (d) | 18.33 [18.31, 18.34] | 88.90 [88.49, 89.27] | 147.02 [146.11, 148.45] | 331.41 [328.40, 336.49] | 11.86 [11.84, 11.87] | 43.17 [43.07, 43.29] |
| K (m/s) | 0.81 [0.57, 0.81] | 0.60 [0.42, 0.70] | 0.69 [0.56, 0.84] | 1.09 [0.94, 1.28] | 0.34 [0.24, 0.50] | 0.53 [0.36, 0.64] |
| e | 0.27 [0.05, 0.31] | 0.25 [0.04, 0.41] | 0.29 [0.11, 0.43] | 0.05 [0.00, 0.11] | 0.20 [0.01, 0.35] | 0.17 [0.01, 0.27] |
| ω (rad) | 6.74 [5.75, 7.22] | 4.41 [3.64, 5.10] | 4.68 [4.11, 5.52] | 3.24 [0.91, 5.64] | 0.77 [–1.47, 2.05] | 0.55 [–1.60, 1.91] |
| M0 (rad) | 2.26 [1.56, 3.07] | 4.69 [3.89, 5.60] | 2.52 [1.76, 3.46] | 4.02 [1.00, 5.72] | 2.74 [0.96, 4.74] | –1.67 [–2.87, 1.68] |
| msini (M⊕) | 2.82 [2.02, 2.92] | 3.52 [2.51, 4.10] | 4.77 [3.91, 5.73] | 10.26 [8.79, 12.15] | 1.03 [0.73, 1.52] | 2.52 [1.69, 3.04] |
| a (au) | 0.127 [0.126, 0.128] | 0.364 [0.360, 0.368] | 0.509 [0.503, 0.515] | 0.875 [0.865, 0.886] | 0.095 [0.094, 0.096] | 0.225 [0.222, 0.227] |
|
|
||||||
| a (m s-1 yr-1) | b (m s-1) | c1 (m s-1) | c2 (m s-1) | c3 (m s-1) | sJ (m s-1) | w 1 |
| –0.52 [–0.64, –0.47] | –1.69 [–2.02, –1.12] | –0.07 [–0.13, 0.01] | 0.02 [–0.01, 0.06] | 0.93 [0.82, 1.06] | 0.89 [0.87, 0.92] | 0.41 [0.37, 0.44] |
|
|
||||||
| w 2 | w 3 | w 4 | ln(τ) (day) | d1 (m s-1) | d2 (m s-1) | d3 (m s-1) |
| 0.23 [0.20, 0.28] | 0.19 [0.14, 0.23] | 0.14 [0.07, 0.16] | –2.06 [–2.37, –1.75] | –0.15 [–0.20, –0.13] | –0.35 [–0.40, –0.31] | –0.40 [–0.46, –0.36] |
|
|
||||||
| d4 (m s-1) | d5 (m s-1) | |||||
| –0.36 [–0.42, –0.31] | –0.23 [–0.28, –0.19] | |||||
Notes. The parameters are estimated in the 6-planet Keplerian solution. The uncertainties of parameters are represented by the values determined at 1% and 99% of the cumulative posterior density. We estimate the minimum planetary mass and semimajor axis using a stellar mass of 0.813 
(Ramírez et al. 2013). Among the parameters of the noise model, c1, c2 and c3 are linear coefficients for S-index, BIS and FWHM, respectively.
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