Table 2
Keplerian parameters of the ε Cyg binary system, from the single- and double-Keplerian models.
| Single-Keplerian | Double-Keplerian | |||||
|---|---|---|---|---|---|---|
| Stellar comp. | Stellar comp. | Planetary comp. | ||||
| Parameter | MCMC | Best-fit | MCMC | Best-fit | MCMC | Best-fit |
| P [days] |  |
19618.6 |  |
19575.7 | 291.1 ± 0.1 | 291.2 |
| M0 [deg](a) | 160.8 ± 1.2 | 160.9 | 159.7 ± 0.9 | 160.4 |  |
129.2 |
| e | 0.9295 ± 0.0003 | 0.9295 | 0.9295 ± 0.0002 | 0.9297 |  |
0.173 |
| ω [deg] | 275.30 ± 0.06 | 275.29 | 275.36 ± 0.06 | 275.38 |  |
276.24 |
| K [m s−1] | 4600.7 ± 1.7 | 4600.9 | 4607.3 ± 1.8 | 4607.5 |  |
30.3 |
| f(m) [Mjup](b) | 10.411 ± 0.016 | 10.407 | 10.390 ± 0.016 | 10.386 |  |
8.366 × 10−7 |
| msini [Mjup](c) | 278 ± 7 | 278 |  |
277 | 1.02 ± 0.06 | 1.04 |
| a [AU] | 15.8 ± 0.2 | 15.8 | 15.7 ± 0.2 | 15.8 | 0.89 ± 0.01 | 0.89 |
Notes. (a) The mean anomalies are calculated at the first observational epoch in the data set of McMillan, t0 = 2 446 945.9465 JD. (b) The expression f(m) denotes the mass function: 
.
(c) Masses and errors have been derived by solving the mass function numerically for fixed inclinations
i of
90°, taking the uncertainty of the primary mass M*
into account.
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