Table 5.
Parameters resulting from the Bayesian analysis as function of the RL filling factor, x.
| x | io | R1 | M1 | M2 | M1/M2 | a | RRL, p,1 | RRL, p,2 | vgrav, 1 | L1/L⊙ | d | Aelli, 1 | Airra |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (deg) | (R⊙) | (M⊙) | (R⊙) | (km s−1) | (kpc) | (mmag) | |||||||
| 1.0 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| 0.9 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| 0.8 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| 0.7 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| 0.6 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| 0.5 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
Notes. The given numbers are the modes and the highest density intervals with probability 0.6827 (see Bailer-Jones et al. 2018 for details on this measure of uncertainty) of the posterior PDFs computed via Monte Carlo integration. Corner plots and posterior PDFs for io, R1, M1, and M2 are shown in Fig. A.2. The quantity a = 0.106 ± 0.006 R⊙ (1 + M1/M2)/sin(io) is the semimajor axis of the binary system, RRL, p,1 and RRL, p,2 are the RL radii of the visible and unseen component at pericenter passage, vgrav, 1 = GM1/(R1c) is the gravitational redshift (G is the gravitational constant, c is the speed of light), L1/L⊙ = (R1/R⊙)2(Teff/T⊙)4 is the luminosity, d = 2R1/Θ is the distance, and Aelli, 1 and Airra are estimates for the expected V-band semi-amplitudes caused by ellipsoidal deformation and irradiance effects, respectively.
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