We present the results of the analysis of the internal velocity dispersions, σv, for the sample of 16 distant galaxy clusters (0.17<~z<~0.55) provided by the Canadian Network for Observational Cosmology (CNOC). Different σv estimates are provided, all based on an interloper-removal algorithm that is different from that originally applied by Carlberg et al. We find that all such methods provide σv estimates that are consistent within less than 10% among themselves and with the original estimates provided by the CNOC collaboration. This result points in favor of a substantial robustness of currently applied methods for optical studies of the internal cluster dynamics. The resulting distribution of velocity dispersions is used to trace the redshift evolution of the cluster abundance with the aim of constraining the matter density parameter, Ωm. We find that constrains on Ωm are very sensitive to the adopted value of σ8=σ8Ωαm (α~=0.4-0.5), as constrained by the local cluster abundance. We find that, as σ8 varies from 0.5 to 0.6, the best fitting density parameter varies in the range 0.3<~Ωm<~1.0. A further source of uncertainty in constraining Ωm is the uncertainties in the correction for the σv-incompleteness of the CNOC sample. This calls attention to the need to better understand the constraints of local cluster abundance and to increase the statistics of distant clusters in order to suppress the systematics related to the sample completeness criteria.
