... systems

Table 1 and Appendices A-C are only available in electronic form at http://www.aanda.org

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... systems

Some of the systems considered in this study are actually hierarchical triple systems. For simplicity, we refer to the whole sample as binaries.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... 15 systems

The radial velocity variations of one of the stars listed in E04 (HD 219542B) was shown to be due to the activity jitter of the star and not to a planet (Desidera et al. 2004).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... binaries

Some planets have been announced after the submission of this paper and they are not considered in this study. One of them is orbiting a component of a wide binary (ADS 16402B; Bakos et al. 2006b). The binary separation is 1550 AU. The two transiting planets discovered by Collier Cameron et al. (2006) have companions candidates discovered using adaptive-optics imaging, whose physical association to the planet hosts needs confirmation.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... stars

The large eccentricity of HD 41004Ba is uncertain ( $e=0.74\pm0.20$).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... binaries

The definition of close binaries used by Pfahl & Muterspaugh (2006) (semimajor axis less than 50 AU) is different to that adopted here.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... measurements

The available observational constraints did not allow Lagrange et al. (2006) to derive a unique solution for the binary orbit. The orbit listed in Table 1 is a plausible, representative solution.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... age

The difference between the kinematic and activity age of GL 86 was previously noted by Rocha Pinto et al. (2002).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... objects

The relative abundances of Allende Prieto et al. (2004) ([O/Fe] = +0.21, [Mg/Fe] = +0.13, [Si/Fe] = +0.08, [Ca/Fe] = +0.18, [Ti/Fe] = +0.11, [Eu/Fe] = +0.30) fit fairly well the expected abundance pattern for a thick star of the metallicity of Gl86, those by Gilli et al. (2006) and Ecuvillon et al. (2006) are more ambiguous ([O/Fe] = -0.01, [Mg/Fe] = +0.21, [Si/Fe] = -0.02, [Ca/Fe] = -0.10, [Ti/Fe] = +0.19). Valenti & Fischer (2005) find an abundance ratio similar to that of Allende Prieto et al. (2004) for two elements ([Si/Fe] = +0.11, [Ti/Fe] = +0.10).

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... J. Schneider

www.exoplanet.eu

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.