Table 1.
Overview of the known multiplicity properties of our sample of WNE stars together with the results of our RV measurements.
| WR# | Spectral type | Binary status | Period | e | ΔRV | σRV | ΔRV > C | |
|---|---|---|---|---|---|---|---|---|
| (GCWR) | (GCWR) | this work | (d) | (km s−1) | (km s−1) | |||
| 1 | WN4 | SB1? | – | – | – | 37.5 | 8.6 | No |
| 2 | WN2 | VB | VB (l) | – | – | 36.9 | 8.3 | No |
| 3 | WN3ha | SB2 | – | – (a) | – | 5.0 | 1.8 | No |
| 6 | WN4b | SB1 | SB1 | 3.8 (b) | 0.1 (b) | 170.0 | 40.3 | Yes |
| 7 | WN4b | – | – | – | – | 33.3 | 10.8 | No |
| 10 | WN5h | VB | VB (l) | – | – | 9.9 | 3.6 | No |
| 110 | WN5b | – | – | – | – | 31.8 | 11.3 | No |
| 127 | WN3b + O9.5V | SB2 | SB2 | 9.5550 ± 0.0002 (c) | 0.04 ± 0.02 (c) | 332.0 | 108.9 | Yes |
| 128 | WN4(h) | SB2?, VB | VB (l) | – | – | 9.7 | 2.8 | No |
| 133 | WN5o + O9I | SB2, VB | SB2, VB (l) | 112.780 ± 0.036 (d) | 0.3558 ± 0.0050 (d) | 111.6 | 25.8 | Yes |
| 138 | WN5o + O9V (e) | SB2, VB | SB2, VB (l) | 1521.2 ± 35 (f) | 0.3 (g) | 92.1 | 29.4 | Yes |
| 139 | WN5o + O6III-V | SB2 | SB2 | 4.212435 (h) | 0.036 ± 0.009 (h) | 618.3 | 168.9 | Yes |
| 141 | WN5o + O5V-III | SB2 | SB2 | 21.6895 ± 0.0003 (i) | 0.018 ± 0.035 (i) | 209.8 | 66.5 | Yes |
| 151 | WN4o + O5V | SB2 | SB2 | 2.12691 d (j) | 0 (fixed) (j) | 650.0 | 220.7 | Yes |
| 152 | WN3(h) | – | – | – | – | 8.3 | 2.6 | No |
| 157 | WN5o + (B0.7II + B1III) (k) | VB | SB3?, VB (l) | – | – | 11.8 | 3.6 | No |
Notes. ΔRV and σRV are calculated in this work and are used to identify tentative spectroscopic binaries. The spectral types are taken from the GCWR unless indicated otherwise. The binary status of this work is reported based on the spectroscopic observations.
Moffat et al. (1986) reported a period of 46.8 d, but it is not supported by our analysis (Appendix A),
Marchenko et al. (1994) [fixed P; 4.212435 d],
(l)VB status carried over from the GCWR.
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