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 5

Overview of derived slopes of the mass function binning the data into 12 bins containing approximately the same number of stars.

Isochrone name	Segment^a	No. of stars	n_i^b	m_min	m_max	α^c	Δα_fit^d	Δα_binning^e
				(M_⊙)	(M_⊙)

3 Myr Padova	NE + SW	220	18–19	5.5	65.8	−1.72	0.09	0.03
4 Myr Padova	NE + SW	261	21–22	4.6	46.7	−1.68	0.09	0.01
5 Myr Padova	NE + SW	289	24–25	4.0	34.5	−1.55	0.09	0.01
4 Myr Geneva	NE + SW	261	21–22	4.5	47.3	−1.77	0.09	0.01

3 Myr Padova	NE	99	8–9	5.5	65.8	−1.76	0.13	0.07
4 Myr Padova	NE	119	9–10	4.6	46.5	−1.73	0.13	0.02
5 Myr Padova	NE	132	11	4.0	34.5	−1.63	0.13	0.00
4 Myr Geneva	NE	119	9–10	4.5	47.3	−1.82	0.13	0.03

3 Myr Padova	SW	121	10–11	5.5	65.6	−1.68	0.13	0.01
4 Myr Padova	SW	142	11–12	4.6	51.0	−1.65	0.12	0.01
5 Myr Padova	SW	157	13–14	4.0	36.2	−1.52	0.12	0.01
4 Myr Geneva	SW	142	11–12	4.5	48.1	−1.70	0.12	0.01

Notes.

^(a)

Segment in the proper motion diagram (Fig. 6).

^(b)

Number of stars per bin.

^(c)

Average of the slopes derived for 1000 realizations of randomly distributing the remainder of the division of the number of stars by the number of bins into the bins by increasing the number of stars in the selected bin by one.

^(d)

Formal uncertainty of the linear fit.

^(e)

Maximum difference between the slopes due to the random distribution of the surplus stars.

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