Table 1
Observed stars.
| id | sp. type | 13/14-06-2009 | 10-08-2009 | 09-07-2010 | 10-07-2010 | Δvmax |
|
|
||||||
| W56 | B0 Ia | −2.6 ± 1.3 | – | 0.1 ± 0.8 | 2.5 ± 1.7 | 5.1 ± 2.9 |
| W13 | B0.5 Ia | spectroscopic binaryb | ||||
| W238 | B1 Iab | 1.2 ± 1.5 | – | −1.4 ± 0.5 | 0.2 ± 1.1 | 2.6 ± 2.0 |
| W23a | B2 Ia | 0.6 ± 0.8 | – | 1.9 ± 0.7 | −2.5 ± 1.3 | 4.4 ± 1.9 |
| W2a | B2 Ia | −5.2 ± 1.1 | −1.1 ± 0.6 | – | 6.3 ± 1.2 | 11.5 ± 2.3 |
| W11 | B2 Ia | 4.6 ± 0.8 | – | −6.5 ± 0.4 | 1.9 ± 0.8 | 11.1 ± 1.0 |
| W28 | B2 Ia | 5.7 ± 0.8 | −5.7 ± 0.8 | – | – | 11.3 ± 1.7 |
| W71 | B2.5 Ia | −5.9 ± 0.5 | 5.9 ± 0.5 | – | – | 11.8 ± 1.0 |
| W70 | B3 Ia | −6.2 ± 0.8 | 6.2 ± 0.8 | – | – | 12.3 ± 1.5 |
| W57a | B4 Ia | 0.4 ± 0.2 | −3.3 ± 0.4 | 1.1 ± 0.5 | 1.8 ± 0.4 | 5.1 ± 0.5 |
| W33 | B5 Ia+ | 6.4 ± 0.8 | 1.2 ± 1.1 | −7.6 ± 0.6 | – | 14.1 ± 0.8 |
| W7 | B5 Ia+ | −4.0 ± 0.5 | 2.7 ± 0.9 | – | 1.3 ± 0.6 | 6.7 ± 1.3 |
| W16a | A5 Ia+ | 4.7 ± 0.2 | −1.4 ± 0.4 | – | −3.3 ± 0.5 | 8.0 ± 0.6 |
| W243a | LBV | −0.5 ± 0.3 | −0.5 ± 0.2 | 1.0 ± 0.3 | – | 1.6 ± 0.6 |
| W12aa | F1 Ia+ | −0.7 ± 0.4 | 1.2 ± 0.2 | – | −0.4 ± 0.4 | 1.9 ± 0.5 |
| W4a | F3 Ia+ | −2.4 ± 0.2 | 2.4 ± 0.2 | – | −0.1 ± 0.2 | 4.8 ± 0.4 |
| W265a | F1-5 Ia+ | −1.2 ± 0.3 | 2.0 ± 0.2 | – | −0.8 ± 0.2 | 3.2 ± 0.5 |
| W32a | F5 Ia+ | −1.8 ± 0.1 | 1.8 ± 0.1 | – | – | 3.6 ± 0.3 |
| W8aa | F8 Ia+ | −0.8 ± 0.1 | −0.4 ± 0.1 | 1.1 ± 0.1 | – | 1.9 ± 0.2 |
| W237 | M3 Ia | 0.7 ± 0.6 | −1.0 ± 0.5 | 0.3 ± 1.0 | – | 1.7 ± 0.5 |
| W26 | M5-6 Ia | 0.6 ± 0.2 | −0.2 ± 0.1 | −0.5 ± 0.3 | – | 1.1 ± 0.5 |
| W9 | sgB[e] | 0.5 ± 0.4 | – | −0.4 ± 0.4 | −0.1 ± 0.2 | 0.9 ± 0.7 |
Notes. The table includes the id of the star from Westerlund (1987), updated by Clark et al. (2005) (Col. 1), its spectral type (Negueruela et al. 2010; Clark et al. 2010) (Col. 2), the deviation in the velocities measured for a single epoch from the average velocity of that star (Cols. 3–5), and the maximum velocity difference between two epochs (Col. 6). All velocities are in km s-1. The relative velocities have been plotted in Fig. 2.
These stars were been included in our sample to calculate the radial velocity dispersion (Sect. 3.2).
See Ritchie et al. (2010) for a discussion of the spectroscopic binary W13.
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