Table 2
Best-fit parameters for the LTT orbits of RZ Dra corresponding to Fig. 3.
| Parameter | Two-LTT | Unit | ||
|
|
||||
| τ1 (i = 1) | τ2 (i = 2) | |||
|
|
||||
|
12.75 | − | ||
|
|
||||
| rms | 535 | s | ||
|
|
||||
| T 0 | 2 444 177.56292 ± 1.1 × 10-5 | BJD | ||
| P 0 | 0.5508761461 ± 5.1 × 10-10 | days | ||
| ab,isinIb,i | 0.34 ± 0.03 | 1.90 ± 0.05 | AU | |
| eb,i (or e1,2) | 0.82 ± 0.27 | 0.62 ± 0.42 | − | |
| ω b,i | 129 ± 33 | 325 ± 56 | deg. | |
| T b,i | 2 443 429 ± 212 | 2,441,573 ± 325 | BJD | |
| Pb,i (or P1,2) | 11 479 ± 5883 | 28 807 ± 8921 | days | |
|
|
||||
| misinIi | 0.07 ± 0.01 | 0.40 ± 0.12 | M ⊙ | |
| aisinIi | 13.9 ± 5.31 | 26.6 ± 5.81 | AU | |
| e i | 0.82 ± 0.27 | 0.62 ± 0.42 | − | |
| ω i | 309 ± 33 | 145 ± 56 | deg | |
| P i | 11 479 ± 5883 | 28 807 ± 8921 | days | |
Notes. Subscripts 1 and 2 refer to the circumbinary companions with i = 1, the inner, and i = 2, the outer, companions. rms measures the root-mean-square scatter of the data around the best-fit model. Uncertainties for the companion’s semi-major axis (aisinIi) have been derived from Kepler’s third law using the largest uncertainty. The mass of the companions was held constant in the error propagation.
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