All Figures

$\begin{figure} \par {\includegraphics[width=15cm,clip]{2740fig1.ps} } \end{figure}$ Figure 1: Distribution of the COCD clusters over magnitude of the brightest star among the most probable cluster members a), over number of most probable members in a cluster b), over angular radius of a cluster c). The hatched histograms in b) and c) are for core radii, whereas the filled histograms are related to corona radii. For convenience, long tails in the distributions in b) and c) are truncated.
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In the text

$\begin{figure} \par {\includegraphics[angle=270,width=13cm,clip]{2740fig2.ps} }\end{figure}$ Figure 2: Example of the spatial, kinematical and evolutionary parameters of the new open cluster ASCC 13. Left upper panel is a sky map of the cluster neighbourhood. The small circles are stars, their size indicates stellar magnitude (only in this panel). In all other diagrams stars are shown as grey dots. The error bars indicate the rms-errors in the corresponding data for $1\sigma$ -members. The large circles in the sky map outline the cluster core (solid) and corona (dashed). The cross indicates the cluster center. The upper right panel is the CMD of the cluster. Bold circles show the stars used for the calculation of the average age of the cluster. The curves are: the empirical ZAMS (leftmost), the red edge of the MS (thick line to the right), the isochrone corresponding to the calculated age, and the limits of the evolved MS (light curves). The legend within the CMD displays the derived parameters of the cluster. The lower left panel shows radial profiles of the projected density. The curves ( from the top to the bottom) correspond to all stars, all members, $1\sigma$ -members. Vertical lines mark the core (solid) and cluster radii (dashed), respectively. The middle panel is the vector point diagram of proper motions. The two rightmost panels are "magnitude equation'' ( $\mu _{x,y}-V$ relation) diagrams, showing the proper motion of cluster members as a function of magnitude. The horizontal lines show the average proper motion of the cluster.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=13cm,clip]{2740fig3.ps} }\end{figure}$ Figure 3: Open clusters identified with ASCC-2.5 data: the comparison of previously known (COCD) and newly discovered (COCD Extension) clusters. Panel a) shows the distribution of clusters over the sky. The crosses indicate known clusters, the circles are for newly discovered ones. Histograms b)- f) are normalised to the number of known clusters ( $N_{\rm tot}=520$ ), the filled and hatched histograms are for known and newly discovered clusters, respectively. Panel b) is the distribution of clusters over the magnitude $V_{\rm b}$ of the brightest $1\sigma$ -member. Panel c) shows the distribution over the number of $1\sigma$ -members in a cluster, whereas panels d)- f) are the distributions of clusters over angular radius, distance and age, respectively. For convenience, long tails in c)- e) are truncated.
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In the text