Abstract
In this work we approximate the quintessence —a measure of the variation of density of dark energy through cosmic time— by a second Chebyshev polynomial that fits several observational data: angular luminosity, luminosity distance, the Hubble parameter. The number density of the “cosmogenic” neutrinos that one should observe today depends on the adiabatic expansion of the Universe (thus on the quintessence) thus it will be determined in the (100 PeV; 10 EeV) energy range for different types of Universe.
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