We present numerical simulations for energy spectra and angular distributions of nucleons above 10 ^ { 19 } eV injected by the radio-galaxy Centaurus A at a distance 3.4 Mpc and propagating in extra-galactic magnetic fields in the sub-micro Gauss range .
We show that field strengths B \simeq 0.3 \mu { G } , as proposed by Farrar & Piran , can not provide sufficient angular deflection to explain the observational data .
A magnetic field of intensity B \simeq 1 \mu { G } could reproduce the observed large-scale isotropy and could marginally explain the observed energy spectrum .
However , it would not readily account for the E = 320 \pm 93 EeV Fly ’ s Eye event that was detected at an angle 136 ^ { o } away from Cen–A .
Such a strong magnetic field also saturates observational upper limits from Faraday rotation observations and X-ray bremsstrahlung emission from the ambient gas ( assuming equipartition of energy ) .
This scenario may already be tested by improving magnetic field limits with existing instruments .
We also show that high energy cosmic ray experiments now under construction will be able to detect the level of anisotropy predicted by this scenario .
We conclude that for magnetic fields B \simeq 0.1 - 0.5 \mu G , considered as more reasonable for the local Supercluster environment , in all likelihood at least a few sources within \simeq 10 Mpc from the Earth should contribute to the observed ultra high energy cosmic ray flux .