Table 1: General data on M 52 and NGC 3960.
  WEBDA Present work  
Cluster $\alpha(2000)$ $\delta(2000)$ Age E(B-V) $d_\odot$   $\alpha(2000)$ $\delta(2000)$ $\ell$ b Age $\mbox{$E(B-V)$ }_{\rm O}$ $d_\odot$ $d_{\rm GC}$ $d_{\rm GC}$
  (hms) ( $^\circ\hbox{$^\prime$ }\hbox{$^{\prime\prime}$ }$) (Myr)   (kpc)   (hms) ( $^\circ\hbox{$^\prime$ }\hbox{$^{\prime\prime}$ }$) ($^\circ$) ($^\circ$) (Myr)   (kpc) (kpc) (kpc)
(1) (2) (3) (4) (5) (6)   (7) (8) (9) (10) (11) (12) (13) (14) (15)

M 52		 23:24:31 +61:35:29 58 0.65 1.42   23:24:42 +61:35:42 112.81 +0.44 $60\pm10$ $\rm0.58^{0.93}_{0.50}$ 1.4 8.7 7.9
NGC 3960 11:50:33 -55:40:24 664 0.30 2.26   11:50:38.9 -55:40:48 294.38 +6.18 $1100\pm100$ $\rm0.13^{0.34}_{0.03}$ 1.7 7.5 6.7
Notes. $\mbox{$E(B-V)$ }\rm _O$ is the colour excess of the cluster's central region (Sect. 3.3), while the bounds refer to the range of reddening throughout the cluster field. Uncertainty in  $\mbox{$E(B-V)$ }\rm _O$ is of the order of $\pm $0.05. Column 14: $d_{\rm GC}$ calculated using $R\rm _O=8.0$ kpc (Reid 1993) as the distance of the Sun to the Galactic center. Column 15: $d_{\rm GC}$ using $R\rm _O=7.2$ kpc (Bica et al. 2006). Uncertainties in $d_\odot$ and  $d_{\rm GC}$ are of the order of $\pm $0.2 kpc.

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