All Tables

Table 1: The barium syndrome among YSyS. The spectral type of the cool component is taken from Mürset & Schmid (1999), or references therein. In column labelled ``nebula'', ``y'' means that an optical nebula has been detected, and ``PN'' that, based on its emission line spectrum, the star has traditionally been included in planetary nebulae catalogues, even though no optical nebula may be visible. The column labelled "P'' lists the orbital period, from Mürset & Schmid (1999).
Table 2: Stars classified as metal-deficient barium stars by Mennessier et al. (1997). The absolute magnitude M_V is a maximum likelihood estimate obtained by Mennessier et al. (1997), except for the additional stars where it is derived from a straight inversion of the Hipparcos parallax (BD $+75^\circ 348$ ), from a spectroscopic estimate of gravity and an educated guess for the mass (BD + $3^\circ 2688$ ) or from a fit to the M 92 isochrone (CS stars). The column labelled "Ba'' indicates whether detailed chemical analyses have confirmed the Ba nature of the star.
Table 3: Averaged absolute abundances (in the scale where $\log \epsilon$ (H) = 12) and normalized abundances [X/Fe] for HD 148897 (relative to the Sun; Grevesse & Sauval 1998). The standard deviations $\sigma$ and the number of lines used in the analysis (n) are also given. Two sets of abundances from Luck (1991) are given: one is based on a "photometric $\log g$ '' (derived from the absolute magnitude, the effective temperature and an estimate for the stellar mass) and the other on the "spectroscopic $\log g$ '' (Fe I/Fe II ionization balance).
Table 4: Abundances for HD 139409, in the scale where $\log \epsilon$ (H) = 12, and normalized with respect to the solar abundances (Grevesse & Sauval 1998). The standard deviations $\sigma$ and the number N of lines used in the analysis are also given.
Table 5: Binary properties of confirmed or suspected metal-deficient barium stars. The column labeled "Ba'' indicates whether detailed chemical analyses have confirmed the Ba nature of the star. The columns labeled $\chi ^2_{\mu _{\rm HIP} - \mu _{\rm Tyc}}$ and Prob( $\chi ^2 > \chi ^2_{\mu _{\rm HIP} - \mu _{\rm Tyc}})$ provide the $\chi ^2$ (and its associated probability) involved in the comparison of Hipparcos and Tycho-2 proper motions (see text for details). The column "Bin.'' has been set to "y'' if the first kind risk of rejecting the null hypothesis that the Tycho and Hipparcos proper motions are equal is smaller than 10%. The column labeled IAD indicates whether the signature of an orbital motion is present in the Hipparcos Intermediate Astrometric Data, according to the various tests described in the text. The column labeled $\sigma (Vr)$ provides the radial-velocity standard deviation, $\Delta t$ and N correspond to the time span and number of observations, respectively. The columns labeled P and "Ref'' list the orbital period (when available) and the reference for the radial velocity and/or orbital data. The column "Binary'' gives the final binarity diagnostics.
Table 6: Orbital elements for BD +04 $^\circ$ 2466.
Table 7: Individual CORAVEL radial velocities and associated errors for HIP 34795, HIP 58596, HIP 76605, BD + $3^\circ 2688$ and BD +04 $^\circ$ 2466. The last column indicates which one of the two CORAVEL spectrovelocimeters has been used (NO = CORAVEL north at the Observatoire de Haute Provence; SO = CORAVEL south on the Danish 1.54-m telescope at ESO).