Table C.1
Estimated remaining contaminations in the cluster member sample after proper motion and colour selection.
Bin No. | mmina | mmaxa | nf,red,ccb | nf,red,pmc | nf,within ccd | nconte | nM,Kf | nmg | ncont/nmg |
(M⊙) | (M⊙) | ||||||||
|
|||||||||
1 | 4.6 | 7.6 | 6 | 17 | 41 | 14.5 ± 7.2 | 110 | 0.13 ± 0.07 | |
2 | 7.6 | 11.9 | 7 | 26 | 33 | 8.9 ± 4.1 | 47 | 0.19 ± 0.09 | |
3 | 11.9 | 18.0 | 5 | 35 | 38 | 5.4 ± 2.7 | 41 | 0.13 ± 0.07 | |
4 | 18.0 | 26.3 | 2.6 ± 1.8 | 3 | 33 | 0.17 ± 0.21h | |||
5 | 26.3 | 34.6 | 1.0 ± 0.8 | 2 | 25 | 0.12 ± 0.11h | |||
6 | 34.6 | 40.0 | 0.3 ± 0.4 | 1 | 12 | 0.11 ± 0.08h |
Notes.
The initial masses refer to the 4 Myr Padova isochrone (Marigo et al. 2008).
Number of field stars removed solely by the red colour-cut (see left panel Fig. B.1).
Number of field stars removed based on their proper motion within the blue and the red colour-cut.
Number of spectroscopically identified M, K supergiants within the proper motion member sample after the colour-cut.
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