Fitting isochrones to open cluster photometric data - A new global optimization tool

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Table 1:

Results for synthetic clusters studied by the fitting method.
Cluster	$N_{\rm stars}$	Contamination (%)	3 $\sigma_{\rm phot}$ (%)	E(B-V)(mag)	Distance (pc)	$\log(Age)$ (yr)
SC 01	432	0%	1.0	$0.40 \pm 0.01$	$2112 \pm 51$	$8.65 \pm 0.05$
SC 02	480	20%	1.0	$0.40 \pm 0.01$	$2062 \pm 43$	$8.71 \pm 0.05$
SC 03	444	50%	1.0	$0.38 \pm 0.01$	$2073 \pm 30$	$8.70 \pm 0.07$
SC 04	65	0%	1.0	$0.38 \pm 0.02$	$2008 \pm 94$	$8.70 \pm 0.07$
SC 05	113	20%	1.0	$0.40 \pm 0.03$	$2060 \pm 60$	$8.75 \pm 0.06$
SC 06	61	50%	1.0	$0.40 \pm 0.02$	$2102 \pm 58$	$8.70 \pm 0.07$

Notes. Synthetic clusters were generated with parameters $\log$ (age) = 8.70 yr, distance = 2100 pc, E(B-V) = 0.40, Z = 0.019) and $N_{\rm stars}$ , including the given contamination fraction and photometric accuracy of 3 $\sigma_{\rm phot}$ .

Source LaTeX | All tables | In the text

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