Table 2.
Identifier, spectral type, and kinematic properties of the runaways and O stars originating from NGC 6611.
| Identifier | Spectral type | |ΔvT| | vR | tkin | Porb | Ref. |
|---|---|---|---|---|---|---|
| – | – | km s−1 | km s−1 | Myr | days | – |
| Runaway O stars | ||||||
| BD–14° 5040 (a) | O5.5 V(n)((f)) | 53 ± 1 | – | 1.04–1.10 | – | 1 |
| UCAC2 27149134 (a) | O3-4 V (c) | 24 ± 1 | – | 1.05–1.19 | – | – |
| HD 168504 | O7.5 V(n)z | 8.7 ± 0.8 | 5 ± 5 | 1.41–1.88 | – | 1 |
| BD–13° 4927 | O7 II(f) | 6.8 ± 0.4 | 20 ± 4 | 0.00–0.27 | – | 2 |
| HD 168183 | O9.5 III + B3-5 V/III | 4.6 ± 0.3 | 19.2 ± 1.0 | 0.83–2.02 | 4 | 2 |
| LS IV –13 14 | O9 V | 3.4 ± 0.2 | 19 ± 5 | 0.00–0.87 | – | 3 |
| W161 | O8.5 V | 2.6 ± 0.2 | –6 ± 5 | 0.32–1.37 | – | 3 |
| HD 168137 (b) | O7 V + O8 V | 2.8 ± 0.3 | 26.3 ± 9.2 | 0.17–1.29 | 1836 | 2,4 |
| B or later-type runaway stars | ||||||
| 4097041394751405184 | B/A (c) | 78 ± 3 | – | 1.26–1.31 | – | – |
| LS IV –14 51 | B0-2 V (c) | 30 ± 1 | – | 1.45–1.57 | – | – |
| W583 | B9 III | 14.1 ± 0.6 | –1 ± 5 | 0.30–0.45 | – | 3 |
| W290 | B2.5 V | 6.0 ± 0.3 | 8 ± 5 | 0.51–1.04 | – | 3 |
| Candidate dynamically interacted O stars | ||||||
| BD–13° 4929 | O7 V + (B0.5 V + B0.5 V) | 5.5 ± 0.5 | 15 ± 2 | – | undef. + (4?) | 2 |
| W222 | O7 V((f)) | 1.5 ± 0.2 | 16 ± 5 | – | – | 3 |
| HD 168075 | O6.5 V((f)) + B0-1 V | 1.0 ± 0.2 | 17 ± 10 | – | 44 | 2,5 |
| HD 168076 | O3.5 V((f+)) + O7.5 V | – | 10 ± 2 | – | ≳105? | 2 |
| Other O stars | ||||||
| W584 (b) | O9 V | 1.2 ± 0.2 | 6 ± 5 | – | – | 3 |
| BD–13° 4930 | O9.5 Vp | 0.7 ± 0.2 | 5 ± 1 | – | – | 2 |
| BD–13° 4928 | O9.5 V | 0.3 ± 0.2 | 17 ± 15 | – | – | 2 |
| BD–13° 4923 | O4 V((f+)) + O7.5 V | – | 3.4 ± 5.3 | – | 13 | 2 |
Notes. We first give the runaway O stars and B or later type runaways. We also give the O stars which could have had dynamical interactions in the past, as well as the remaining O stars. Each sub-table is sorted by |ΔvT|.
References. (1) Maíz Apellániz et al. (2016); (2) Sana et al. (2009, 2012); (3) Evans et al. (2005); (4) Le Bouquin et al. (2017); (5) Barbá et al. (2010).
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