All Tables

Table 1: $\gamma$ Doradus stars candidates observed at OHP showing LPV. The first 2 columns give the HD or HIP star number (if this latter exists). Asterisked stars are both good $\gamma$ Doradus candidates and possible members of binary systems (see Sect. 5). Next columns respectively provide the number of spectra, the observation window, the mean exposure time, the mean S/N value, the number of photometric frequencies previously detected, the LPV signature, remarks about the binarity, the $v~\sin i$ value and some references $^{\dag }$ .
Table 2: $\gamma$ Doradus star candidates observed at OHP not showing LPV. The first 2 columns give the HD or HIP star number (if this latter exists). Next columns respectively provide the number of spectra, the observation window, the mean exposure time, the mean S/N value, the status of their $\gamma$ Dor variability (BF: Bona fide; PC: prime candidate; COROT: possible COROT target chosen as a $\gamma$ Doradus candidate from its spectral type), the number of photometric frequencies previously detected, general remarks, the $v~\sin i$ value and some references $^{\dag }$ .
Table 3: Parameters of the binary orbit for the SB2 star HD 62454. Our data together with those of Kaye et al. (1999) lead to a final rms of the residuals of 1.81 km s^-1.
Table 4: Parameters of the binary orbit for the star HD 70645. The final rms of the residuals is 2.32 km s^-1. Note that we have only used here the velocities computed from a Gaussian fit.
Table 5: Parameters of the binary orbit for the star HD 80731. The final rms of the residuals is 2.61 km s^-1. Note that we have only used here the velocities computed from a Gaussian fit.
Table 6: Parameters of the binary orbit for the star HD 100215. Because we have too scarce data, the eccentricity has been arbitrarily set to zero. Consequently, the longitude of the periastron is not given. The final rms of the residuals is 1.35 km s^-1. Note that we have only used here the velocities computed from a Gaussian fit.
Table 7: Parameters of the binary orbit for the SB2 star HD 221866. The final rms of the residuals is 2.28 km s^-1.
Table 8: List of stars for which the main HIPPARCOS frequency could be deduced (3 ${\rm rd}$ column, in d^-1) and fitted to our spectroscopic data, with its corresponding amplitude (4 ${\rm rd}$ column, in mmag). Then the next columns respectively provide the corresponding radial velocity amplitude [km s^-1] computed from a sine-fit with the f-frequency (together with the associated fraction of the variance this frequency accounts for), and then the total velocity range [km s^-1] measured. Finally, last column provides the $2K/\Delta m$ amplitudes ratio values [km s^-1 mag^-1].
Table 9: Same as Table 8, but for stars for which the combined fit of photometric and spectroscopic data is not possible. Light amplitude [mmag] and/or radial velocity ranges [km s^-1] are given.