Self-consistent physical parameters for five intermediate-age SMC stellar clusters from CMD modelling

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Volume 561 (January 2014)

A&A, 561 (2014) A106

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Table 3

Structural parameters derived from King profile fitting, as described in Sect. 2.3.

Cluster	n _field	n ₀	r _c	r _t	c	Overdensity
	(stars/′′²)	(stars/′′²)	(′′)	(′′)	log (r_t/r_c)	(n₀ − n_field)/(n_field)

AM 3 – original	0.0014	0.072 ± 0.009	21.6 ± 1.4	65 ± 6	0.48 ± 0.05	50
AM 3 – completed	0.0018	0.150 ± 0.015	18.1 ± 1.1	62 ± 6	0.54 ± 0.05	82
Lindsay 2 – original	0.0061	0.11 ± 0.05	41 ± 8	85 ± 17	0.31 ± 0.12	17
Lindsay 2 – completed	0.0078	0.25 ± 0.05	29.8 ± 3.2	74 ± 9	0.39 ± 0.07	31
HW 1 – original	0.0162	0.114 ± 0.009	17.2 ± 1.3	49.2 ± 3.0	0.46 ± 0.04	6
HW 1 – completed	0.0204	0.349 ± 0.021	14.7 ± 0.8	55.3 ± 3.7	0.58 ± 0.04	16
Lindsay 3 – original^a	0.0116	0.057 ± 0.011	–	–	–	3.9
Lindsay 3 – completed	0.0155	0.238 ± 0.010	16.4 ± 0.5	89 ± 8	0.73 ± 0.04	14
HW 40 – original	0.0195	0.096 ± 0.019	16.6 ± 2.3	69 ± 17	0.62 ± 0.12	4
HW 40 – completed	0.0249	0.28 ± 0.04	17.8 ± 1.6	65 ± 9	0.56 ± 0.7	10
HW 34 – original^a	0.0444	0.069 ± 0.012	–	–	–	0.5
HW 34 – completed^a	0.0960	0.212 ± 0.021	–	–	–	1.2

Notes. The overdensity column indicates how much bigger the central density is with respect to the field density.

^(a)

Cases where fits did not converge, and we attribute the density of the innermost region of the profile as n₀ to estimate a lower limit of the overdensity.

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