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Table 3
Comparison between the binary and triple system scenarios for WR 133.
| Feature | Binary system scenario | Triple system scenario |
|---|---|---|
| Detection of non-thermal emission despite a strong free–free absorption. | Difficult to reconcile with the measurement of a thermal spectrum across the 112.4-d orbit. | The larger size of an eccentric outer orbit should allow the detection of non-thermal emission at some epochs. |
| Switch between detection and non-detection of non-thermal emission with a time interval of several years. | Difficult to explain in the context of the 112.4-d orbit considering the lack of detection in our sampling of the orbit. | May be explained by an eccentric outer orbit with observations closer to periastron passage in July 2014 and September 2015. |
| Lack of evidence for a third object in the system. | In favor of the binary system scenario. | Not in favor of the triple system scenario, but provides loose constraints on the nature of the hypothetical third object, and previous studies are not sufficient to completely reject the existence of a third star. |
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