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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.

(a)

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.

(b)

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).

(c)

The microturbulence of HIP 103019 was calculated following the expression presented in Adibekyan et al. (2012a).

(d)

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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