The Gzk Feature in the Spectrum of Ultra High Energy Cosmic Rays

The detection of the GZK feature in the cosmic ray spectrum, resulting from the production of pions by ultra-high energy protons scattering off the cosmic microwave background (CMB), can shed light on the mysterious sources of these high energy particles. Using numerical simulations we developed for the propagation of Ultra High Energy Cosmic Rays (UHECR) in the CMB we determine the statistical significance of the GZK feature in the spectrum of UHECR measured by AGASA and HiRes and we show that, with the small sample of events with energies ∼ 10 eV detected thus far, an accurate and statistically significant determination of the GZK feature is not possible. The data from these two experiments are best fit by two different injection spectra in the region below 10 eV, and a comparison of the spectra suggests the presence of about a 30% systematic errors in the relative energy determination. Correcting for these systematics, the two experiments are best fit by the same injection spectrum in the region below 10 eV, while above this threshold they maintain their disagreement, but only at the 2σ level. These results clearly show the need for much larger experiments such as Auger, EUSO and OWL, that can increase the number of detected events by one or two orders of magnitude making the determination of the GZK feature feasible.