All Tables

Table 1: Log of the observations used in this study.
Table 2: Number of stars observed (N) and mean internal errors ( $\sigma$ ) as a function of apparent visual magnitude.
Table 5: Comparison of the V magnitude to the published broadband data.
Table 6: Distribution parameters and their uncertainties from a 9-parametric Gaussian model applied to M 67 cluster and the field. $n_{\rm c}$ measures the volume of the cluster frequency function ( $n_{\rm f} = 1- n_{\rm c}$ ), $\mu _x$ and $\mu _y$ are the mean relative proper motions, $\sigma _{\rm c}$ , and $\sigma _{\mu _x}$ and $\sigma _{\mu _y}$ are the dispersions of the Gaussians fitted to the cluster and field distributions, and $\rho$ is the correlation for the field function (it fixes the orientation of the field elliptical function). The units of $\mu$ and $\sigma$ are mas yr^-1.
Table 8: The cross-identification of stars considered as candidate members by us, with the radial velocities sudies by Mathieu et al. (1990,1986) and the comparison of those with the parametric ( $P_{\rm P}$ ) and non-parametric ( $P_{\rm NP}$ ) probabilities. See text for explanation of the agreement index $P_{\rm c}$ .
Table 9: The same as Table 8, for stars considered as non-members by us.
Table 10: The cross-identification of known multiple star systems and their astrometric segregation from this work (last column). First column is our identification number (Table 3), second column that from BDA and third that from Sanders (1977).
Table 11: Our BS candidates in M 67, and their photometry. First column is our identification number (Table 3), second column that from BDA, and third that from Sanders (1977). Last column gives the astrometric membership (void values for stars without astrometric membership determination).