Table 3: Coefficients of the calibration equations.
$b_1 = 3.465 \pm 0.009$ $b_2 = 0.25 \pm 0.02$ $b_3 = -0.145 \pm 0.008$

$v_1 = 3.244 \pm 0.005$ $v_2 = 0.16 \pm 0.02$ $v_3 = 0.021 \pm 0.005$

$v_{1,i} = 3.244 \pm 0.005$ $v_{2,i} = 0.16 \pm 0.02$ $v_{3,i} = 0.009 \pm0.005$

$i_1 = 4.097 \pm 0.005$ $i_2 = 0.08 \pm 0.02$ $i_3 = 0.006 \pm 0.005$

**Table 3:** Coefficients of the calibration equations.
$b_1 = 3.465 \pm 0.009$	$b_2 = 0.25 \pm 0.02$	$b_3 = -0.145 \pm 0.008$
$v_1 = 3.244 \pm 0.005$	$v_2 = 0.16 \pm 0.02$	$v_3 = 0.021 \pm 0.005$
$v_{1,i} = 3.244 \pm 0.005$	$v_{2,i} = 0.16 \pm 0.02$	$v_{3,i} = 0.009 \pm0.005$
$i_1 = 4.097 \pm 0.005$	$i_2 = 0.08 \pm 0.02$	$i_3 = 0.006 \pm 0.005$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data reduction
	3 Astrometry
	4 Star counts and cluster size
	5 Colour-magnitude diagrams
	6 Cluster fundamental parameters
	7 Conclusions
	References