Table 3: Comparison of our results with the literature data on King's parameters for the clusters in common.
Cluster Present paper Literature
  n2 $r_{\rm fit}$ $r_{\rm c}$ $r_{\rm t}$ $M_{\rm c}$ N* $r_{\rm area}$ $r_{\rm c}$ $r_{\rm t}$ note ref
    deg pc $m_\odot$   deg pc    
Pleiades 219 14 $1.4\pm0.1$ $20.5\pm1.3$ $3107\pm638$ 270 6 $1.4\pm0.5$ $16\pm7$   1
            1067 3 0.9...2.9 13.1 a 2
            1200 10 2.1...2.8 12.4...14.5 b 3
Praesepe 154 9 $0.8\pm0.1$ $17.1\pm1.2$ $1806\pm428$ 185 4 $1.0\pm0.5$ $11.1\pm4.9$   4
             1000 3.8 3.5 16 c 5
NGC 2168 186 1.95 $1.8\pm0.2$ $17.9\pm2.3$ $724\pm677$   0.47 1.3...4.3 $8.35...\infty$   6
NGC 2477 10 0.55 $1.9\pm1.0$ $6.5\pm1.2$ $89\pm51$   0.25 1.8 8.1 d 7
Notes: (a) - $r_{\rm c}$ was computed for member groups of different mass, $r_{\rm t}$ was derived from the cluster mass via Eq. (3); (b) - $r_{\rm c},~r_{\rm t}$ were obtained from the distribution of low-mass stars ( $m<1~m_\odot$); the original results are given in angular units and were transformed to linear sizes by us; (c) - $r_{\rm c},~r_{\rm t}$ were obtained from the distribution of low-mass stars ( $m<1~m_\odot$); (d) - the area is a square of $0.5\times0.5$ sq.deg.
References: 1 - Raboud & Mermilliod (1998a), 2 - Pinfield et al. (1998), 3 - Adams et al. (2001), 4 - Raboud & Mermilliod (1998b), 5 - Adams et al. (2002), 6 - Leonard & Merritt (1989), 7 - Eigenbrod et al. (2004).

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