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Impact of the magnetic horizon on the interpretation of the Pierre Auger Observatory spectrum and composition data

Journal Article · · JCAP
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  1. Adelaide U.
  2. LIP, Lisbon
  3. OATo, Turin; INFN, Turin
  4. Centro Atomico Bariloche
  5. NIKHEF, Amsterdam; Vrije U., Amsterdam; Nijmegen U., IMAPP; Cracow, INP
  6. ITeDA, Buenos Aires; U. Tech. Natl., Argentina
  7. Gran Sasso; INFN, Aquila; L'Aquila U.
  8. Santiago de Compostela U., IGFAE
  9. Catania U.; INFN, Catania; Messina U.
  10. Lehman Coll.
  11. ITeDA, Buenos Aires
  12. Milan U.; INFN, Milan
  13. INFN, Naples; Naples U.
  14. Aachen, Tech. Hochsch.
  15. Turin U.; INFN, Turin
  16. Bath U.
  17. Pierre Auger Observ.
  18. L'Aquila U.; INFN, Aquila
  19. Prague, Inst. Phys.
  20. Colorado School of Mines
  21. Adelaide U.; San Augustin Natl. U., Arequipa
  22. LPSC, Grenoble
  23. Cracow, INP
  24. Bonn, Max Planck Inst., Radioastron.
  25. IFIR, Rosario
  26. KIT, Karlsruhe, ETP; ITeDA, Buenos Aires
  27. Nijmegen U., IMAPP; NIKHEF, Amsterdam; Vrije U., Amsterdam
  28. IJCLab, Orsay; IUF, Paris
  29. KIT, Karlsruhe, IAP; Pierre Auger Observ.
  30. ICAS, UNSAM, Buenos Aires; Rio de Janeiro Federal U.
  31. Campinas State U.
  32. Colorado State U.
  33. Granada U.
  34. Vrije U., Brussels
  35. Messina U.; INFN, Catania; Catania U.
  36. Chiapas Autonoma U.
  37. ITeDA, Buenos Aires; Natl. Tech. U., San Rafael
  38. Sao Paulo U., Sao Carlos
  39. INFN, Lecce
  40. Palacky U.
  41. Naples U.; INFN, Naples
  42. IJCLab, Orsay
  43. INFN, Milan; Milan Polytechnic
  44. INFN, Lecce; Salento U.
  45. Niteroi, Fluminense U.
  46. Case Western Reserve U.
  47. Siegen U.
  48. La Plata U.; Buenos Aires, CONICET
  49. Buenos Aires, CONICET; CEFIMAS, Buenos Aires
  50. Rio de Janeiro Federal U.
  51. ITeDA, Buenos Aires; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  52. IFMT, Caceres
  53. KIT, Karlsruhe, IAP; Pierre Auger Observ.; ITeDA, Buenos Aires
  54. INFN, Turin
  55. Bucharest U.
  56. Mexico U., ICN
  57. Rio de Janeiro, CBPF; LIP, Lisbon
  58. Rio de Janeiro, CBPF
  59. Parana U.
  60. KIT, Karlsruhe, ETP; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  61. Nijmegen U., IMAPP; ASFYON; Amsterdam U.; NIKHEF, Amsterdam; Vrije U., Amsterdam
  62. New York U. (main)
  63. KIT, Karlsruhe, IPE
  64. KIT, Karlsruhe, IAP; Pierre Auger Observ.; ASI, Rome
  65. Michigan Tech. U.
  66. Stefan Inst., Ljubljana; Nova Gorica U.
  67. Delaware U.
  68. Nijmegen U., IMAPP
  69. Chicago U., EFI; Osaka City U.
  70. Wuppertal U.
  71. Aachen, Tech. Hochsch.; Erlangen - Nuremberg U., ECAP
  72. UEFS, Feira de Santana
  73. KIT, Karlsruhe, ETP
  74. Fermilab
  75. KIT, Karlsruhe, IAP; Pierre Auger Observ.; Vrije U., Brussels
  76. Bucharest, Inst. Space Science
  77. CEFET, Rio de Janeiro
  78. ABC Federal U.
  79. LPNHE, Paris
  80. Wisconsin U., Madison
  81. Nova Gorica U.
  82. Brussels U., IIHE
  83. USTC, Hefei; Palermo U.; Messina U.; INFN, Catania
  84. Puebla U., Inst. Fis.
  85. NASA, Goddard
  86. Rome U., Tor Vergata; INFN, Rome2
  87. Charles U.
  88. Santander Industrial U.
  89. CINVESTAV, IPN
  90. Campina Grande Federal U.
  91. Sao Paulo U.
  92. L'Aquila U.
  93. NIKHEF, Amsterdam; Vrije U., Amsterdam; Nijmegen U., IMAPP
  94. Chicago U., EFI
  95. Hamburg U., Inst. Theor. Phys. II
  96. Buenos Aires, CONICET
  97. INFN, Rome2
  98. Vrije U., Brussels; Kapteyn Astron. Inst., Groningen
  99. Delaware U.; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  100. IASF, Palermo; Messina U.; INFN, Catania
  101. Bucharest U.; Nijmegen U., IMAPP
  102. Vrije U., Brussels; Brussels U., IIHE
  103. Penn State U.
  104. INFN, Milan; Milan U.; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  105. Lodz U.
  106. Medellin U.
  107. Amsterdam U.
  108. Nova Gorica U.; Stefan Inst., Ljubljana
+ Show Author Affiliations
The flux of ultra-high energy cosmic rays reaching Earth above the ankle energy (5 EeV) can be described as a mixture of nuclei injected by extragalactic sources with very hard spectra and a low rigidity cutoff.Extragalactic magnetic fields existing between the Earth and the closest sources can affect the observed CR spectrum by reducing the flux of low-rigidity particles reaching Earth. We perform a combined fit of the spectrum and distributions of depth of shower maximum measured with the Pierre Auger Observatory including the effect of this magnetic horizon in the propagation of UHECRs in the intergalactic space.We find that, within a specific range of the various experimental and phenomenological systematics, the magnetic horizon effect can be relevant for turbulent magnetic field strengths in the local neighbourhood in which the closest sources lieof order B$$_{rms}$$ ≃ (50–100) nG (20 Mpc/d$$_{s}$$)( 100 kpc/L$$_{coh}$$)$$^{1/2}$$, with d$$_{s}$$ the typical intersource separation and L$$_{coh}$$ the magnetic field coherence length. When this is the case,the inferred slope of the source spectrum becomes softer and can be closer to the expectations of diffusive shock acceleration, i.e., ∝ E$$^{-2}$$.An additional cosmic-ray population with higher source density and softer spectra, presumably also extragalactic and dominating the cosmic-ray flux at EeV energies, is also required to reproduce the overall spectrum and composition results for all energies down to 0.6 EeV.
Research Organization:
ABC Federal U.; ASFYON; ASI, Rome; Aachen, Tech. Hochsch.; Adelaide U.; Amsterdam U.; Bath U.; Bonn, Max Planck Inst., Radioastron.; Brussels U., IIHE; Bucharest U.; Bucharest, Inst. Space Science; Buenos Aires, CONICET; CEFET, Rio de Janeiro; CEFIMAS, Buenos Aires; CINVESTAV, IPN; Campina Grande Federal U.; Campinas State U.; Case Western Reserve U.; Catania U.; Centro Atomico Bariloche; Charles U.; Chiapas Autonoma U.; Chicago U., EFI; Colorado School of Mines; Colorado State U.; Cracow, INP; Delaware U.; Erlangen - Nuremberg U., ECAP; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Gran Sasso; Granada U.; Hamburg U., Inst. Theor. Phys. II; IASF, Palermo; ICAS, UNSAM, Buenos Aires; IFIR, Rosario; IFMT, Caceres; IJCLab, Orsay; INFN, Aquila; INFN, Catania; INFN, Lecce; INFN, Milan; INFN, Naples; INFN, Rome2; INFN, Turin; ITeDA, Buenos Aires; IUF, Paris; KIT, Karlsruhe, ETP; KIT, Karlsruhe, IAP; KIT, Karlsruhe, IPE; Kapteyn Astron. Inst., Groningen; L'Aquila U.; LIP, Lisbon; LPNHE, Paris; LPSC, Grenoble; La Plata U.; Lehman Coll.; Lodz U.; Medellin U.; Messina U.; Mexico U., ICN; Michigan Tech. U.; Milan Polytechnic; Milan U.; NASA, Goddard; NIKHEF, Amsterdam; Naples U.; Natl. Tech. U., San Rafael; New York U. (main); Nijmegen U., IMAPP; Niteroi, Fluminense U.; Nova Gorica U.; OATo, Turin; Osaka City U.; Palacky U.; Palermo U.; Parana U.; Penn State U.; Pierre Auger Observ.; Prague, Inst. Phys.; Puebla U., Inst. Fis.; Rio de Janeiro Federal U.; Rio de Janeiro, CBPF; Rome U., Tor Vergata; Salento U.; San Augustin Natl. U., Arequipa; Santander Industrial U.; Santiago de Compostela U., IGFAE; Sao Paulo U.; Sao Paulo U., Sao Carlos; Siegen U.; Stefan Inst., Ljubljana; Turin U.; U. Tech. Natl., Argentina; UEFS, Feira de Santana; USTC, Hefei; Vrije U., Amsterdam; Vrije U., Brussels; Wisconsin U., Madison; Wuppertal U.
Sponsoring Organization:
US Department of Energy
Grant/Contract Number:
89243024CSC000002; AC02-07CH11359
OSTI ID:
2426470
Report Number(s):
FERMILAB-PUB-24-0144-CSAID-PPD-TD-V; oai:inspirehep.net:2774194; arXiv:2404.03533
Journal Information:
JCAP, Journal Name: JCAP Vol. 07
Country of Publication:
United States
Language:
English

Figures / Tables (15)

Figure 1(p. 8)figure Figure 1
Table 1(p. 10)table Table 1
Figure 2(p. 11)figure Figure 2
Table 2(p. 12)table Table 2
Figure 3(p. 13)figure Figure 3
Figure 4(p. 14)figure Figure 4
Figure 5(p. 15)figure Figure 5
Table 3(p. 16)table Table 3
Figure 6(p. 17)figure Figure 6
Table 4(p. 18)table Table 4
Figure 7(p. 19)figure Figure 7
Figure 8(p. 20)figure Figure 8
Figure 9(p. 22)figure Figure 9
Table 5(p. 22)table Table 5
Figure 10(p. 23)figure Figure 10

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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
cosmic ray experiments
cosmic ray theory
ultra high energy cosmic rays