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|
|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|
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.
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.
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