Table 1.
Combined multiplicity properties from spectroscopy (literature) and interferometry (this work) for our sample of 39 WRs.
| WR | Total | Single | Unresolved | Resolved | Resolved | Total WRs | Observed |
|---|---|---|---|---|---|---|---|
| class | stars | Stars | spectroscopic companions | spectroscopic companions | wide companions | with companions | multiplicity fraction |
| WNh | 13 | 10 | 2 | 0 | 1 | 3 | 0.23 ± 0.12 |
| WN | 11 | 5 | 3 | 2 | 1 | 6 | 0.55 ± 0.15 |
| WNL | 6 | 3 | 0 | 2 | 1 | 3 | 0.50 ± 0.20 |
| WNE | 5 | 2 | 3 | 0 | 0 | 3 | 0.60 ± 0.22 |
| WC | 15 | 9 | 1 | 4 | 2 ( * ) | 6 | 0.40 ± 0.13 |
| cWR | 26 | 14 | 4 | 6 | 3 | 12 | 0.46 ± 0.10 |
| All WR | 39 | 24 | 6 | 6 | 4 | 15 | 0.38 ± 0.08 |
Notes.
Rows are divided into WNh, WN, and WC, with WN further divided into WNL and WNE. The last column lists the observed multiplicity fraction along with errors calculated using binomial statistics (( * )as WR 48 is a triple candidate, it is counted twice).
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