GZK cutoff distortion due to the energy error distribution shape

Astroparticle Physics

Volumn 25, Issue 6, 2006, Pages 375-379

  Albuquerque, Ivone F M ^a,b   Smoot, George F ^c  

^a UNIVERSITY OF SÃO PAULO   (Brazil)

^b UNIVERSITY OF CALIFORNIA   (United States)

^c LAWRENCE BERKELEY NATIONAL LABORATORY   (United States)

Author keywords

Cosmic rays; Energy error distribution; GZK cutoff; Ultra high energy

Indexed keywords

COSMIC RAYS; DISTORTION (WAVES); ELECTRON ENERGY LEVELS; ERROR ANALYSIS; ESTIMATION; MEASUREMENT ERRORS; NORMAL DISTRIBUTION; REGRESSION ANALYSIS;

ENERGY ERROR DISTRIBUTION; GZK CUTOFF; LOGNORMAL DISTRIBUTION; ULTRA HIGH ENERGY;

HIGH ENERGY PHYSICS;

EID: 33745213745     PISSN: 09276505     EISSN: None     Source Type: Journal    
DOI: 10.1016/j.astropartphys.2006.03.010     Document Type: Article

References (20)

1. Greisen K. Phys. Rev. Lett. 16 (1966) 748
2. Zatsepin G.T., and Kuźmin V.A. Pis'ma Zh. Eksp. 4 (1966) 114
3. Zatsepin G.T., and Kuźmin V.A. JETP Lett. 4 (1966) 78
4. Chung D.J.H., Farrar G.F., and Kolb E.W. Phys. Rev. D 57 (1998) 4606
5. Albuquerque I.F.M., Farrar G.F., and Kolb E.W. Phys. Rev. D 59 (1999) 015021
6. Elbert J.W., and Sommers P. Astrophys. J. 441 (1995) 151
7. Takeda M., et al. Astropart. Phys. 19 (2003) 447
8. Takeda M., et al. Phys. Rev. Lett. 81 (1998) 1163
9. R.U. Abbasi et al. Available from: astro-ph/0501317 (2005).
10. de Marco D., Blasi P., and Olinto A.V. Astropart. Phys. 20 (2003) 53
11. T. Stanev. Available from: astro-ph/0303123 (2003).
12. Available from: .
13. Gaisser T. Cosmic Rays and Particle Physics (1990), Cambridge University Press
14. Pierre Auger Project Design Report. Available from: .
15. AIRES package (Airshower Extended Simulations v.2.6.0), S.J. Sciutto. Available from: astro-ph/0106044; .
16. C.O. Escobar, L.G. Santos, R.A. Vazquez. Available from: astro-ph/0202172 (2002).
17. Blanton M., Blasi P., and Olinto A.V. Astropart. Phys. 15 (2001) 275 In this paper it is shown that at ultra high energies an isotropic cosmic ray flux does not differ much from a flux originated from a distribution compatible with the one observed from large scale structure
18. Blumenthal G. Phys. Rev. D 1 (1970) 1596
19. Geddes J., Quinn T.C., and Wald R.M. Astrophys. J. 459 (1996) 384
20. Berezinsky V.S., and Grigore'va S.I. Astron. Astrophys. 199 (1988) 1