Table 6
O and B stars with proper motions departing from the bulk of the sample in Cygnus OB2.
| O Star | SpT | μα | μδ | v sin i | B19 group | Comments |
|---|---|---|---|---|---|---|
| A46 | O7 V((f)) | −4.7975 ± 0.0401 | −6.5080 ± 0.0445 | 75 | 2 | |
| A15 | O7 Ibf | −6.6917 ± 0.1052 | −3.0674 ± 0.1075 | 270 | 2 | X−ray emission(a) |
| A37 | O5 V((f)) | +4.7680 ± 0.0660 | +2.5090 ± 0.0743 | 225 | 2 | Stellar bowshock nebulae candidate(b,c) |
| MT91−5 | O6.5 V((f))z | +1.7037 ± 0.7238 | −8.2103 ± 0.6239 | 70 | − | X-ray emission(a) |
| A26 | O9.5 IV | −0.9824 ± 1.4337 | −4.5861 ± 1.6144 | 85 | − | X-ray emission(a) |
| A20 | O7 III((f)) | 1.4764 ± 0.7290 | −6.2771 ± 0.6385 | 80 | − | X-ray emission(a) |
| Cyg OB2 #22B | O6 IV((f)) | −3.0826 ± 0.1007 | −4.6284 ± 0.7757 | 145 | − | Member of multiple system(d) |
| MT91−516 | O6 IVf | −7.4619 ± 1.5750 | −8.4631 ± 1.6608 | 85 | − | X-ray emission(a) |
| Cyg OB2 #10 | O9.7 Iab | +1.2143 ± 0.8583 | −1.4617 ± 0.7715 | 55 | − | |
| B Star | SpT | μα | μδ | v sin i | B19 group | Comments |
| BD+40°4208 | B1 V | +0.765 ± 0.055 | −2.64 ± 0.053 | 165 | 0 | v sin i from (e) |
| J20331029+4123446 | B4 II-III | −6.761 ± 0.043 | −7.248 ± 0.045 | − | 1 | |
| Cyg OB2 #4B | B0:V ne | −2.991 ± 0.048 | +0.742 ± 0.055 | − | 1 | |
| BD+40°4193 | B2 V | −0.397 ± 0.049 | −2.387 ± 0.059 | 70 | 1 | v sin i from (e) |
| Schulte 30 | B2 IIIe | −0.001 ± 0.043 | −2.51 ± 0.044 | 182 | 1 | v sin i from (f) |
| A39 | B2V | +0.048 ± 0.054 | −3.009 ± 0.058 | 200 | 1 | v sin i from (e) |
| J20303833+4010538 | B1 V | −0.05 ± 0.044 | −3.829 ± 0.047 | 255 | 2 | v sin i from (e) |
| J20325440+4115219 | B3 V | −1.4434 ± 0.6728 | +3.5137 ± 0.7639 | − | − | X-ray emission(a) |
| J20313364+4136046 | B3 V | −0.2003 ± 0.3608 | −6.6582 ± 0.3415 | − | − | |
| J20333979+4122523 | B1 V | −5.2397 ± 0.7872 | −3.2279 ± 0.6934 | 142 | − | v sin i from (f) |
Notes. Proper motions are given in milliarcseconds per year. For O stars, spectral types and projected rotational velocities (in kilometers per second) come from this work. For B stars, we list spectral types given by Comerón & Pasquali (2012); Berlanas et al. (2018a,b) and v sin i values from the literature, whenever available. Stars with poor RUWE values have no B19 group assigned. Stars included in group 3 (foreground and background objects) are not actually runaway candidates and, thus, they are not listed.
References. (a) Rauw et al. (2015); (b) Kobulnicky et al. (2016); (c)Kobulnicky et al. (2017); (d)Maíz Apellániz (2010); (e)Berlanas et al. (2018b); (f)Wolff et al. (2007).
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