All Tables

Table 1: a) Measured line intensities, relative to I(C IV-5806) = 100, and FWHM (C IV-5806 and C III-5696) obtained for 42 WR CSPNe. The symbol "B'' indicates that the line results from a blend. The measured values for C IV-5806 are given in Col. 23 (units 10^-15 ergs/cm²/s). All measurements are based on observations made at the 1.52 m telescope at ESO ( $\lambda \lambda$ 370-750 nm). Objects marked $^{\circ }$ were also observed at the 3.6 m telescope at ESO ( $\lambda \lambda$ 432-600 nm), the corresponding measurements are shown in italics. Objects marked * were observed at OHP ( $\lambda \lambda$ 510-600 nm). The symbol "(c)'' means that the line was detected by a visual inspection of plates obtained at the 1.52 m telescope + Chilicass at ESO, in Aug. 1972 (exposure time: 4h). The symbols ":'' and "vis'' mean respectively that the measurements are of poor quality, and that the line is visible but not measurable. The symbol "A'' refers to absorption features.
Table 1: b) Dereddened line intensities relative to I(C IV-5806) = 100, obtained for 42 WR CSPNe.
Table 2: Classification criteria based on dereddened line intensities relative to C IV-5806 = 100 for 42 CSPNe. The ratio also studied by CMB98 are shown in italics.
Table 3: Stellar parameters of the 42 analysed CSPNe. A mean value of the stellar temperatures and $V\infty$ is given for each subtype. For SwSt1 (PN G 1.5-6.7) the mark * refers to the text. Uncertain and very uncertain values are followed by ":" and "::'' respectively.
Table 4: List of all known WC and wels stars. The PN labelled with "S'' belongs to the Sagittarius dwarf galaxy. Spectral classes marked with "*'' are classified based on observations obtained at OHP (1993-2000, see Sect. 2). *1: visual inspection on "Pediscou'' plates, obtained at OHP (tel 1.93m), in June 1974 with an exposure time of 15 min. *2: visual inspection on "electronic camera'' plates, obtained at OHP (tel 1.93m), in 1961, by M. Chopinet (private communication).
References stand for: AOS92 = Acker et al. (1992); AGC96 = Acker et al. (1996); Al76 = Aller (1976); AK85 = Aller & Keyes (1985); CMB98 = Crowther et al. (1998); CG73 = Cesco & Gibson (1973); CJA87 = Chu et al. (1987); CJ87 = Cohen & Jones (1987); DH91 = Dong & Hu (1991); F99 = Feibelman (1999); GS02 = Gorny & Siodmiak (2002); HB90 = Hu & Bibo (1990); HS70 = Hack & Struve (1970); Ha96 = Hamann (1996a); He82 = Heap (1982); HCLS81 = van der Hucht et al. (1981); KH97 = Koesterke & Hamann (1997a, 1997b); KS84 = Kaler & Shaw (1984); KSFI91 = Kaler et al. (1991); LH98 = Leuenhagen & Hamann (1998); LHJ94 = Leuenhagen et al. (1994); LHJ96 = Leuenhagen et al. (1996); LSB00 = Liu et al. (2000); Lu77 = Lutz (1977); Lu78 = Lutz (1978); M91 = Méndez (1991); MN79 = Méndez & Niemela (1979); MN82 = Méndez & Niemela (1982); MPC03 = Morgan et al. (2003); MPR01 = Morgan et al. (2001); P03 = Parker (2003); PM03a = Parker & Morgan (2003a); PM03b = Parker & Morgan (2003b); PMH01 = Parker et al. (); PAS98 = Parthasarathy et al. (1998) (see the text); PSM98 = Peña et al. (2001); PSM01 = Peña et al. (2001); SA69 = Smith & Aller (1969); TAS93 = Tylenda et al. (1993); V88 = Volk (1988); W75 = Webster (1975).