The present-day mass function of the Quintuplet cluster based on proper motion membership

B. Hußmann; A. Stolte; W. Brandner; M. Gennaro; A. Liermann

doi:10.1051/0004-6361/201117637

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Volume 540 (April 2012)

A&A, 540 (2012) A57

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Table C.1

Estimated remaining contaminations in the cluster member sample after proper motion and colour selection.

Bin No.	m_min^a	m_max^a	n_f,red,cc^b	n_f,red,pm^c	n_{f,within cc}^d	n_cont^e	n_M,K^f	n_m^g	n_cont/n_m^g
	(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 ± 0.21^h
5	26.3	34.6				1.0 ± 0.8	2	25	0.12 ± 0.11^h
6	34.6	40.0				0.3 ± 0.4	1	12	0.11 ± 0.08^h

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 n_cont and n_M,K (see text).

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