Table 3.
Combined orbital solutions and dynamical masses.
| Circular solutions | Eccentric solutions | |||
|---|---|---|---|---|
| astro + RVpre-sd + KBe | astro + RVs | astro + RVpre-sd + KBe | astro + RVs | |
| P [d] | 40.3270 ± 0.0012 | 40.3266 ± 0.0016 | 40.32640 ± 0.00094 | 40.3261 ± 0.0013 |
| T0 [RJD] | 53117.276 ± 0.073 | 53117.295 ± 0.094 | 53220.49 ± 0.74 | 53220.6 ± 1.0 |
| e | 0.0 | 0.0 | 0.0288 ± 0.0043 | 0.0289 ± 0.0058 |
| a″ [mas] | 1.298 ± 0.013 | 1.299 ± 0.017 | 1.283 ± 0.011 | 1.284 ± 0.015 |
| i [°] | 39.86 ± 0.84 | 39.9 ± 1.2 | 39.38 ± 0.69 | 39.37 ± 0.95 |
| Ω [°] | 26.0 ± 2.0 | 25.5 ± 2.7 | 25.7 ± 1.5 | 25.4 ± 2.1 |
| ωBe [°] | 90 | 90 | 111.2 ± 6.6 | 111.9 ± 9.0 |
| KBe [km s−1] | 3.9 ± 0.7 (a) | 3.87 ± 0.26 | 3.9 ± 0.7 (a) | 3.90 ± 0.27 |
| Kpre-sd [km s−1] | 60.55 ± 0.68 | 60.72 ± 0.90 | 61.07 ± 0.66 | 61.15 ± 0.88 |
| γ [km s−1] | 7.02 ± 0.50 | 7.56 ± 0.19 | 7.28 ± 0.49 | 7.57 ± 0.19 |
| a [AU] | 0.3728 ± 0.0086 | 0.374 ± 0.011 | 0.3794 ± 0.0079 | 0.3800 ± 0.0093 |
| q = Mpre-sd/MBe | 0.064 ± 0.012 | 0.0638 ± 0.0045 | 0.064 ± 0.012 | 0.0638 ± 0.0044 |
| Mtotal [M⊙] | 4.26 ± 0.30 | 4.28 ± 0.36 | 4.49 ± 0.28 | 4.51 ± 0.33 |
| MBe [M⊙] | 4.00 ± 0.26 | 4.03 ± 0.34 | 4.22 ± 0.25 | 4.24 ± 0.31 |
| Mpre-sd [M⊙] | 0.258 ± 0.054 | 0.270 ± 0.056 | 0.270 ± 0.056 | 0.270 ± 0.027 |
| d [pc] | 287.3 ± 7.2 | 287.6 ± 8.9 | 295.6 ± 6.6 | 296.0 ± 8.0 |
| rms astrometry [μas] | 25 | 25 | 19 | 19 |
| rms RVBe [km s−1] | 1.64 | 1.53 | 1.56 | 1.53 |
| rms RVpre-sd [km s−1] | 4.92 | 4.96 | 4.83 | 4.85 |
Notes. The relative astrometry (astro) is given in Table A.1. The pre-sd RVs and KBe were taken from Gies & Wang (2020). P is the orbital period, T0 is the epoch of periastron or the epoch of the superior conjunction, e is the eccentricity, a″ is the angular semimajor axis of the orbit, i is the orbital inclination, Ω is the longitude of the ascending node, ω is the longitude of the periastron (fixed at 90° for circular orbits), K are the velocity semiamplitudes for the two components, γ is the systemic velocity, a is the orbital semimajor axis, q = MsdOB/MBe is the mass ratio, Mtotal is the total mass, and MBe and MsdOB are the dynamical masses for the two components. “rms” stands for the rms residuals of specified datasets.
Taken from Gies & Wang (2020).
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