Table 3.
Solutions for star systems resolved by Gaia with direct-imaging data and either HIPPARCOS transit data or literature mass fractions.
| Name | ℳ1 | σℳ1 | ℳ2 | σℳ2 | ϖ | σϖ | ρℳ1, ℳ2 | F2 |
|---|---|---|---|---|---|---|---|---|
| Gl277 | 0.5276 | 0.0046 | 0.2069 | 0.0031 | 83.465 | 0.052 | 0.77 | 3.93 |
| Gl330 | 0.4969 | 0.0247 | 0.3184 | 0.0159 | 61.513 | 0.107 | 0.98 | 3.37 |
| Gl568 | 0.3106 | 0.0067 | 0.2129 | 0.0047 | 87.439 | 0.069 | 0.95 | 1.53 |
| Gl860 | 0.2915 | 0.0062 | 0.1789 | 0.0046 | 248.354 | 1.560 | 0.39 | 3.49 |
| Gl65 (a) | 0.1224 | 0.0012 | 0.1195 | 0.0012 | 371.396 | 0.453 | −0.28 | 1.19 |
| Gl473 (a) | 0.1379 | 0.0023 | 0.1258 | 0.0022 | 227.041 | 0.389 | −0.76 | 1.36 |
Notes.
The masses of the primary ℳ1 and secondary ℳ2 are given in ℳ⊙, the parallax ϖ is given in mas, ρℳ1, ℳ2 is the correlation between the mass estimates, and F2 is the goodness of fit. Solution using the literature mass fraction. The full table including Gaia and HIPPARCOS IDs and full orbital solution is available at the CDS.
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