The "negative values" of the star density in the star clusters structure and method of their removal.

In the case of a small density gradient, large fluctuations in the star density distribution in the region of a thin cluster corona lead to negative values in the spatial star density functions f(r). These values are obtained by Kholopov's numerical method from the visible density function F(r), where r is the distance from the cluster center. A numerical method is presented here for removing the negative densities in f(r) via the smoothing of the F(r) curves. This method preserves all the details of the curves that describe the cluster structure. Results of the application of this method to NGC 2420 are presented.