All Tables

Table 1: Program stars. The first four columns give our identification number (cf. finding chart in Fig. 1), and that assigned by Hoag et al. (1961), Sanders (1973) and Kazlauskas & Jasevicius (1986). V and B-Vare Tycho-2 $V_ {\rm T}$ and $(B-V)_{\rm T}$ transformed into Johnson system following Bessell (2000) prescriptions. U-B is the median of the measurements by Massey et al. (1995), Joshi et al. (1983) and Hoag et al. (1961). Star #10 is reported as a short period variable by Peña et al. (2001).
Table 3: Spectral types of the program stars from Wang & Hu (2000), from photometry in the Vilnius system by Kazlauskas & Jasevicius (1986) transformed by us into spectral types following Strayzis (1977), and from classification of our Echelle spectra against the Yamashita et al. (1977) reference spectral atlas. The last columns give the E_B-V (from Fitzgerald 1970 intrinsic colors) and the spectro-photometric distances for our spectral classification and the photometry in Table 1.
Table 4: Example of the table containing the epoch radial velocities (and their errors) for the program stars, available in full only in electronic form at the CDS.
Table 5: Heliocentric radial velocity (with its standard error) of the program stars, binary status and cluster membership according to radial velocities, and projected rotational velocity (with its standard error). The radial velocity of the binary stars is the barycentric velocity from the orbital solutions in Table 6. The last column gives the projected rotation period $P_{\rm rot}$ / $\sin i$ of the solved binaries to be compared with the orbital period.
Table 6: Orbital solution for the binary stars we discovered in NGC 6913. For binaries #6 and 16 the epoch radial velocities in Table 4 did not allowed a determination of the orbital period and therefore the derivation of the orbit. The errors are given in parenthesis in units of the last digit. The last raw gives the rms deviation of the solution from the observed radial velocities.
Table 7: Cluster membership of program stars from the literature according to astrometric, photometric, and spectral type criteria, and ours based on spectrophotometric parallaxes and radial velocities. The last column gives our final membership status obtained by merging the results of the various criteria. S73 = Sanders (1973), D02 = Dias et al. (2002), C77 = Crawford et al. (1977), J83 = Joshi et al. (1983), W00 = Wang & Hu (2000).
Table 2: Journal of observations. D is the dispersions (Å/pix) at H $\alpha$ (0.19 corresponding to unbinned spectra, 0.38 to 2 $\times$ binned spectra), and $\Delta \lambda$ is the wavelength coverage. The last column gives the program stars observed in each given run (the table is only available in electronic form).