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Fig. 5.


Distribution of peak flux densities in S/N units on the logarithmic scale for the pulsar B0320+39 (left), for transient J0139+33 (right). The vertical axis shows the number of detected pulses, and the horizontal axis shows the S/N of these pulses. The histograms were drawn in increments of three on the abscissa axis. The figure shows that the distributions are different, despite the similar values of the dispersion measures, distances, and flux densities of the strongest observed pulses in the second pulsar B0320+39 and the second transient J0139+33. The lognormal distribution with probable power tail (see the fragment of the figure) was fit for B0320+39, and the broken power dependence was fit for J0139+33 (see the fragment of the figure). Standard deviations are shown in the upper corner of B0320+39.

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