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Table 5

TGAS cluster parallaxes as derived by our two independent procedures.


Bona fide cluster members Loosely selected members VL09 VL17
Cluster r C.L. N ϖ ϵϖ N ϖ ϵϖ σϖ nGauss ϖ ϵϖ ϖ ϵϖ
(deg) σ (mas) (mas) (mas) (mas) (mas) (mas) (mas) (mas) (mas)
NGC 2451A 2 2.0 19 5.293 0.069 25 5.266 0.061 0.504 1 5.45 0.11 5.59 0.11
NGC 2451B 1 1.5 14 2.773 0.089 46 2.763 0.041 0.354 2 2.72a 0.44a
NGC 2516 0.7 1.5 22 2.586 0.063 33 2.588 0.052 0.467 1 2.92 0.10 2.99 0.08
NGC 2547 1.5 1.5 10 2.746 0.091 17 2.720 0.071 0.224 1 2.11 0.17 2.79 0.06
IC 2391 2 2.0 17 6.850 0.064 24 6.829 0.055 0.216 2 6.90 0.12 7.01 0.11
IC 2602 1.5 2.0 17 6.757 0.069 30 6.749 0.051 0.198 1 6.73 0.09 6.74 0.05
IC 4665 1 2.0 10 2.732 0.091 15 2.784 0.073 0.124 2 2.81 0.27 2.83 0.05
NGC 6633 0.7 1.5 17 2.432 0.066 72 2.438 0.032 0.212 2 2.67 0.32 2.37 0.03

Notes. When available, the parallaxes estimated by van Leeuwen (2009) and VL17 are also listed for comparison.

References. (a) From Carrier et al. (1999).

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