The low-mass stellar-mass functions of rich, compact clusters in the Large Magellanic Cloud

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Table 1:

Fundamental parameters of our LMC cluster sample.
Cluster	log(age)^a	E(B-V)^b	(m-M)₀^b	$\log(M_{\rm cl}/M_{\odot})^{c}$	$R_{\rm core}^{c}$	$D_{\rm LMC}^{d}$
	[yr]	(mag)	(mag)		(pc)	( $^{\circ}$ )
NGC 1805	7.65 $\pm$ 0.05	0.04	18.59	3.52 $\pm$ 0.13	1.33 $\pm$ 0.06	3.86-4.00
NGC 1818	7.65 $\pm$ 0.05	0.03	18.58	$\rm 4.13^{+0.15}_{-0.14}$	2.45 $\pm$ 0.09	3.47-3.61
NGC 1831	8.75 $\pm$ 0.05	0.00	18.58	4.81 $\pm$ 0.13	4.44 $\pm$ 0.14	4.82-4.85
NGC 1868	9.00 $\pm$ 0.05	0.02	18.55	4.53 $\pm$ 0.10	1.62 $\pm$ 0.05	5.57-5.47
NGC 2209	9.10 $\pm$ 0.05	0.07	18.39	$\rm 5.03^{+0.36}_{-0.6}$	5.43 $\pm$ 0.33	5.48-5.43
Hodge 14	9.30 $\pm$ 0.05	0.04	18.49	$\rm 4.33^{+0.34}_{-0.28}$	1.80 $\pm$ 0.14	4.19-4.37

Notes: $D_{\rm LMC}$ is the distance from the LMC centre; the two values indicate $D_{\rm LMC}$ to the optical, geometrical centre (Bica et al. 1996) and the dynamical, rotation centre (Westerlund 1990), respectively. References: ^a this paper (the age uncertainties are driven by the discreteness of the Padova isochrones); ^b Castro et al. (2001); ^c Mackey & Gilmore (2003), ^d Meurer et al. (1990).

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