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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. 

(a)

The initial masses refer to the 4   Myr Padova isochrone (Marigo et al. 2008).

(b)

Number of field stars removed solely by the red colour-cut (see left panel Fig. B.1).

(c)

Number of field stars removed based on their proper motion, but redder than the red colour-cut.

(d)

Number of field stars removed based on their proper motion within the blue and the red colour-cut.

(e)

Estimated number of contaminating stars.

(f)

Number of spectroscopically identified M, K supergiants within the proper motion member sample after the colour-cut.

(g)

Number of proper motion cluster members after the colour-cut. Unlike in the final cluster sample, the spectroscopically identified M, K supergiants are not removed.

(h)

The number of contaminants includes ncont and nM,K (see text).

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