$B_7$ should be $\sim 0.3 \div 0.4$. As it is shown in our combined Fig. \[harrari\], such magnetic field has to sweep out some fraction of the southern Galactic hemisphere. However, using the data from SUGAR[^9] which are also plotted into this figure, we are able to show that such a model could not be completely correct. This is due to the fact that these regions with proposed zero particle flux — in contrary to the theoretical expectations — contain several SUGAR events.

Finally, two interesting works treating the turbulent fields appeared recently. [@jaime] carefully analyzed the influence of turbulent fields on possible clustering of UHECRs and [@harari] made large study of properties of typical turbulent fields with respect to amplification and multiplication of source images.

Computer Model {#compres}
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In our simulation we have supposed the conservative Galactic magnetic field model by [@han], which was amended with toroidal and poloidal field components and with turbulent fields linked to spiral arms; this complete configuration of magnetic field was discussed in detail above.

Despite using various types of initial data, we present here only the results for real data. Namely, even such constrained set of data can sufficiently demonstrate all important 