Table 1
Stellar parameters of the CORALIE sample.
| Star | Teff | log g | ξt | [Fe/H] | M2 sin i | References |
| [K] | [dex] | [cm/s] | [dex] | [MJ] | ||
|
|
||||||
| HD 4747 | 5316 ± 50 | 4.48 ± 0.10 | 0.79 ± 0.10 | −0.21 ± 0.05 | 46.1 | 2 |
| HD 52756 | 5216 ± 65 | 4.47 ± 0.11 | 1.11 ± 0.13 | 0.13 ± 0.04 | 59.3 | 1 |
| HD 74014 | 5662 ± 55 | 4.39 ± 0.08 | 1.10 ± 0.07 | 0.26 ± 0.04 | 49.0 | 1 |
| HD 89707 | 6047 ± 42 | 4.52 ± 0.05 | 0.99 ± 0.06 | −0.33 ± 0.03 | 53.6 | 1 |
| HD 167665 | 6224 ± 39 | 4.44 ± 0.04 | 1.18 ± 0.05 | −0.05 ± 0.03 | 50.6 | 1 |
| HD 189310 | 5188 ± 50 | 4.49 ± 0.09 | 0.94 ± 0.10 | −0.01 ± 0.03 | 25.6 | 1 |
| HD 211847 | 5715 ± 24 | 4.49 ± 0.05 | 1.05 ± 0.03 | −0.08 ± 0.02 | 19.2 | 1 |
|
|
||||||
| HD 3277a | 5539 ± 49 | 4.36 ± 0.06 | 0.91 ± 0.07 | −0.06 ± 0.04 | 64.7 | 1 |
| HD 17289a | 5924 ± 32 | 4.37 ± 0.04 | 1.15 ± 0.04 | −0.11 ± 0.03 | 48.9 | 1 |
| HD 30501a | 5223 ± 27 | 4.56 ± 0.08 | 1.18 ± 0.04 | −0.06 ± 0.02 | 62.3 | 1 |
| HD 43848a | 5334 ± 92 | 4.56 ± 0.15 | 1.35 ± 0.17 | 0.22 ± 0.06 | 24.5 | 1 |
| HD 53680a | 5167 ± 94 | 5.37b ± 0.29 | 2.08 ± 0.31 | −0.29 ± 0.04 | 54.7 | 1 |
| HD 154697a | 5648 ± 45 | 4.42 ± 0.05 | 1.04 ± 0.06 | 0.13 ± 0.04 | 71.1 | 1 |
| HD 164427Aa | 6003 ± 27 | 4.35 ± 0.03 | 1.19 ± 0.03 | 0.19 ± 0.02 | 48.0 | 1 |
| HIP 103019a | 4913 ± 115 | 4.45 ± 0.28 | 0.54c ± 0.10 | −0.30 ± 0.06 | 52.5 | 1 |
|
|
||||||
| HD 74842d | 5517 ± 38 | 4.50 ± 0.06 | 1.01 ± 0.06 | −0.08 ± 0.03 | – | 3 |
| HD 94340d | 5902 ± 26 | 4.19 ± 0.03 | 1.30 ± 0.03 | 0.11 ± 0.02 | – | 3 |
| HD 112863d | 5342 ± 36 | 4.57 ± 0.07 | 1.08 ± 0.07 | −0.11 ± 0.03 | – | 3 |
| HD 206505d | 5392 ± 44 | 4.46 ± 0.07 | 1.02 ± 0.07 | 0.11 ± 0.03 | – | 3 |
Notes.
These eight stars have companion minimum masses, mC sin i, in the BD range determined from spectroscopic RV measurements, but are discarded in Sahlmann et al. (2011) using their Hipparcos astrometry.
The surface gravity of the star HD 53680 is unusually high for its derived effective temperature. A significantly lower Teff value (probably <4500 K) is expected from its weak and narrow Hα profile (see Fig. 4 and Sect. 5).
The microturbulence of HIP 103019 was calculated following the expression presented in Adibekyan et al. (2012a).
These four stars, as a comparison sample, are also from the CORALIE sample, but they do not have detected BD companions
Reference. (1) Sahlmann et al. (2011); (2) Santos et al. (2005); (3) This work.
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