High resolution spectroscopic data of a sample consisting of 24 planetary nebulae (PNe) with WR-type nuclei ([WC]) from the list of Tylenda et al. (1993) plus 1 late-[WC] presented by De Marco et al. (2001), and 7 PNe with weak emission line stars (WELS) nuclei listed in Tylenda et al. (1993) are analyzed. The data were collected using the 2.1 m telescope at the Observatorio Astronómico Nacional, San Pedro Mártir, México and were used to determine the expansion velocity (V
) of the gaseous component in each sample object in the following ions: [N II]λA6584, [O II]λ3729, [O III]λA5007, Hβ, HeI λ5876, and HeII λ4686. A sample of 8 non-WR type (typical) PNe were observed as a controlo sample. All observational data were systematically gathered using the REOSC Echelle Spectrograph on 1995 July 29–31, 1996 June 14–17, 1997 August 3–4, 1998 December 11–14, 1999 October 4–7, and 2000 November 1–3. In order to take the highest V
of the gesous component in each ion, it was taken the half width of the line at one tenth of the maximum intensity when the line featured either a single Gaussian profile or a Gaussian with extended wings profile. For two-peaks profiles, V
was measured taking into account both the peak-to-peak displacement and the HW of the lines.