Table 5
Mean proper motions and their errors from Dias et al. (2014) for our cluster sample.
| Cluster | μαcosδ | μ δ | U s | V s | W s |
| (mas yr-1) | (mas yr-1) | (km s-1) | (km s-1) | (km s-1) | |
|
|
|||||
| Scutum: | |||||
| NGC 6603 | 1.06 ± 4.06 | −0.74 ± 5.12 | 4.68 ± 26.75 | 22.11 ± 72.15 | −13.46 ± 69.58 |
| Perseus: | |||||
| King 1 | −2.43 ± 2.59 | 1.02 ± 1.50 | 34.91 ± 44.01 | 17.43 ± 36.75 | 21.55 ± 15.70 |
| NGC 559 | −4.58 ± 2.95 | 1.41 ± 1.46 | 86.82 ± 47.90 | 58.09 ± 52.77 | 5.04 ± 18.88 |
| NGC 7245 | −1.98 ± 3.58 | −1.76 ± 3.19 | 16.99 ± 73.88 | −18.66 ± 45.73 | 16.73 ± 69.93 |
| Outer: | |||||
| Berkeley 23 | 2.65 ± 2.10 | −7.32 ± 4.68 | 9.55 ± 13.39 | −204.98 ± 116.58 | −10.75 ± 78.99 |
Notes. Us, Vs, and Ws are the components of the non-circular velocity at the position of each cluster. They are computed from proper motions and radial velocities using the values for the motion of the Sun with respect to the LSR from Reid et al. (2014) and Galactic rotation as Θ0 = 220 km s-1, R0 = 8.50 kpc, and dΘ/dR = −0.2 km s-1 kpc-1.
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