Table 2
Semi-major axes, inflation factors and reduced chi-squared values for the detected companions.
| Target | a in AU | I | ![$\[\chi_{\mathrm{red}}^2\]$](/articles/aa/full_html/2024/08/aa50018-24/aa50018-24-eq11.png){kind=small} |
|---|---|---|---|
| Gaia DR3 2728129004119806464 B | (0.938 ± 0.023) | 0.4 | 0.04 |
| Gaia DR3 4986031970629390976 B | −(a) | 2.9 | −(a) |
| CD-50 869 B | (2.73 ± 0.28) | 0.2(b) | 3.67 |
| HD 17155 B | (2.07 ± 0.07) | 1.6 | 2.52 |
| WT 766 | (0.676 ± 0.008) | 2.9 | 1.84 |
| Gaia DR3 4739421098886383872 B | (1.500 ± 0.019) | 3.0 | 2.19 |
| Gaia DR3 4858390078077441920 B | (1.265 ± 0.016) | 1.4 | 0.54 |
| StKM1-1494 B | (1.329 ± 0.014) | 1.3 | 0.92 |
Notes. The semi-major axes, a, shown here result from the Gaia-plus-GRAVITY orbital posteriors. The inflation factors, I, are required to make the 1 σ position angle confidence interval encompass the detection. The presented reduced chi-squared values of the best-fit orbital solution were found by means of a gradient descent from the most probable parameter set in the MCMC posterior sampling. (a)Note that G ...0976 B lacks values for the semi-major axis as well as the reduced chi-squared since the posterior could not be sampled for this companion. (b)The inflation factor found for the CD-50 869 system results from a non-Gaussian position angle distribution rendering the value unusable.
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