changes of features of particle flux. These real data[^10] were taken from our catalogue of UHECRs[^11]. We propagate these particles through Galactic magnetic field assuming various charges — starting as protons (proton number $Z = 1$), continuing as oxygen nuclei ($Z = 8$) and ending with iron nuclei ($Z = 26$). All particles were traced back off the influence of Galactic field. The final distance of each particle was assumed to be 40 kpc from Earth. We present here (Figure \[finalfig\]) the results of simulations corresponding the real UHECR data (145 UHECR positions and energies) taken successively as protons, oxygen and iron nuclei.

Results of particle tracking
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We can state that the given deflection ranges (Fig. \[finalfig\]) are in good agreement with previous models ([@stanev1], [@medina] or [@olinto]) of propagation of UHECRs through the Galactic magnetic field. Hence we can formulate the following conclusions:

-   [As we already stressed above, the detail of global structure of GMF is still **uncertain**, but despite that we can claim that its influence is non-negligible for protons and essential for Fe nuclei.]{}

-   [The simulations of particles with higher charges (e.g. oxygen or iron nuclei) are transforming the isotropic distribution to structures, which 