Skip to main content
OSTI.GOVU.S. Department of Energy Office of Scientific and Technical Information
U.S. Department of Energy
Office of Scientific and Technical Information
 

Constraining the sources of ultra-high-energy cosmic rays across and above the ankle with the spectrum and composition data measured at the Pierre Auger Observatory

Journal Article · · JCAP
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [7];  [3];  [8];  [9];  [2];  [10];  [11];  [12];  [13];  [9];  [2];  [14];  [15] more »;  [16];  [17];  [18];  [19];  [20];  [21];  [12];  [5];  [22];  [22];  [23];  [11];  [24];  [17];  [21];  [25];  [17];  [15];  [26];  [27];  [5];  [11];  [11];  [9];  [11];  [28];  [29];  [30];  [31];  [23];  [32];  [33];  [34];  [35];  [36];  [3];  [37];  [38];  [7];  [14];  [27];  [17];  [39];  [1];  [40];  [41];  [42];  [38];  [2];  [24];  [43];  [44];  [14];  [25];  [45];  [46];  [28];  [47];  [48];  [25];  [1];  [45];  [49];  [32];  [50];  [19];  [51];  [27];  [44];  [52];  [44];  [36];  [24];  [53];  [54];  [18];  [27];  [55];  [2];  [56];  [17];  [32];  [57];  [44];  [11];  [6];  [58];  [59];  [60];  [27];  [61];  [61];  [25];  [62];  [9];  [63];  [25];  [42];  [64];  [59];  [6];  [64];  [34];  [40];  [61];  [49];  [18];  [24];  [64];  [65];  [25];  [14];  [9];  [4];  [4];  [14];  [14];  [4];  [66];  [4];  [5];  [3];  [7];  [1];  [41];  [67];  [28];  [53];  [17];  [9];  [47];  [4];  [1];  [25];  [11];  [25];  [32];  [32];  [39];  [39];  [68];  [36];  [69];  [17];  [70];  [17];  [35];  [35];  [25];  [64];  [49];  [25];  [61];  [14];  [71];  [61];  [72];  [11];  [73];  [71];  [74];  [24];  [36];  [2];  [75];  [76];  [71];  [77];  [27];  [17];  [17];  [1];  [78];  [24];  [24];  [34];  [47];  [66];  [79];  [44];  [53];  [75];  [7];  [15];  [25];  [80];  [80];  [81];  [70];  [55];  [55];  [35];  [9];  [61];  [39];  [22];  [34];  [4];  [21];  [35];  [3];  [17];  [32];  [54];  [60];  [35];  [35];  [55];  [9];  [18];  [28];  [62];  [62];  [82];  [82];  [39];  [44];  [83];  [52];  [17];  [9];  [7];  [75];  [35];  [17];  [5];  [84];  [23];  [37];  [49];  [44];  [19];  [15];  [25];  [2];  [9];  [64];  [85];  [79];  [59];  [17];  [62];  [35];  [35];  [9];  [71];  [17];  [7];  [28];  [15];  [64];  [14];  [9];  [78];  [25];  [4];  [86];  [28];  [18];  [64];  [15];  [75];  [87];  [83];  [9];  [37];  [17];  [70];  [2];  [14];  [76];  [25];  [44];  [25];  [24];  [35];  [25];  [71];  [30];  [32];  [17];  [88];  [11];  [25];  [47];  [49];  [89];  [35];  [77];  [78];  [9];  [18];  [18];  [59];  [8];  [8];  [14];  [17];  [18];  [77];  [5];  [21];  [11];  [23];  [66];  [24];  [9];  [90];  [91];  [12];  [85];  [25];  [17];  [37];  [2];  [21];  [14];  [17];  [15];  [47];  [25];  [25];  [39];  [39];  [55];  [41];  [75];  [83];  [25];  [92];  [47];  [87];  [17];  [93];  [77];  [94];  [25];  [25];  [70];  [5];  [35];  [9];  [17];  [66];  [7];  [95];  [63] « less
  1. Adelaide U.
  2. Lisbon, CFTP
  3. OATo, Turin; INFN, Turin
  4. Centro Atomico Bariloche
  5. Cracow, INP
  6. ITeDA, Buenos Aires; U. Tech. Natl., Argentina
  7. Santiago de Compostela U., IGFAE
  8. Lehman Coll.
  9. ITeDA, Buenos Aires
  10. INFN, Naples
  11. Aachen, Tech. Hochsch.
  12. INFN, Turin; Turin U.
  13. Bath U.
  14. Pierre Auger Observ.
  15. L'Aquila U.; INFN, Aquila
  16. Bucharest, Polytechnic Inst.
  17. Prague, Inst. Phys.
  18. Bucharest U.
  19. Gran Sasso; INFN, Aquila; L'Aquila U.
  20. Adelaide U.; Buenos Aires U.
  21. LPSC, Grenoble
  22. Rosario U.
  23. KIT, Karlsruhe, ETP; ITeDA, Buenos Aires
  24. IJCLab, Orsay
  25. KIT, Karlsruhe, IAP; Pierre Auger Observ.
  26. ICAS, UNSAM, Buenos Aires; Rio de Janeiro Federal U.
  27. Campinas State U.
  28. Siegen U.
  29. Granada U.
  30. Vrije U., Brussels
  31. Messina U.; INFN, Catania; USTC, Hefei; Palermo U.
  32. Nijmegen U., IMAPP; NIKHEF, Amsterdam; Vrije U., Amsterdam
  33. Chiapas Autonoma U.
  34. Milan U.; INFN, Milan
  35. Wuppertal U.
  36. Catania U.; INFN, Catania; Messina U.
  37. Sao Paulo U.
  38. INFN, Lecce
  39. Palacky U.
  40. ITeDA, Buenos Aires; Natl. Tech. U., San Rafael
  41. Naples U.; INFN, Naples
  42. Delaware U.
  43. INFN, Milan; Milan, Polytech.
  44. INFN, Lecce; Salento U.
  45. Niteroi, Fluminense U.
  46. Dortmund U.
  47. La Plata U.; Buenos Aires, CONICET
  48. Buenos Aires, IAFE; CEFIMAS, Buenos Aires
  49. ITeDA, Buenos Aires; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  50. Rio de Janeiro Federal U.; Valongo Observ.
  51. IFMT, Caceres
  52. Sao Paulo U., Sao Carlos
  53. KIT, Karlsruhe, IAP; Pierre Auger Observ.; ITeDA, Buenos Aires
  54. INFN, Turin
  55. Mexico U., ICN
  56. Parana U.
  57. KIT, Karlsruhe, ETP; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  58. Nijmegen U., IMAPP; ASFYON; Amsterdam U.; NIKHEF, Amsterdam; Vrije U., Amsterdam
  59. Chicago U., EFI
  60. New York U. (main)
  61. KIT, Karlsruhe, IPE
  62. Michigan Tech. U.
  63. Stefan Inst., Ljubljana; Nova Gorica U.
  64. Nijmegen U., IMAPP
  65. INFN, Milan
  66. Brussels U., IIHE
  67. UEFS, Feira de Santana
  68. KIT, Karlsruhe, IAP; Pierre Auger Observ.; Vrije U., Brussels
  69. Bucharest, Inst. Space Science
  70. Colorado School of Mines
  71. KIT, Karlsruhe, ETP
  72. CEFET, Rio de Janeiro
  73. ABC Federal U.
  74. LPNHE, Paris
  75. Puebla U., Inst. Fis.
  76. Wisconsin U., Madison
  77. Nova Gorica U.
  78. Hamburg U.
  79. USTC, Hefei; Palermo U.; Messina U.; INFN, Catania
  80. Rome U., Tor Vergata; INFN, Rome2
  81. Colorado School of Mines; Wuppertal U.
  82. Charles U.
  83. Santander Industrial U.
  84. CINVESTAV, IPN
  85. NIKHEF, Amsterdam; Vrije U., Amsterdam; Nijmegen U., IMAPP
  86. Buenos Aires, IAFE
  87. INFN, Rome2
  88. Delaware U.; KIT, Karlsruhe, IAP; Pierre Auger Observ.
  89. IASF, Palermo; Messina U.; INFN, Catania
  90. Lodz U.
  91. Medellin U.
  92. Valongo Observ.
  93. Amsterdam U.
  94. Rio de Janeiro Federal U.
  95. Nova Gorica U.; Stefan Inst., Ljubljana
+ Show Author Affiliations
In this work we present the interpretation of the energy spectrum and mass composition data as measured by the Pierre Auger Collaboration above 6 × 10$$^{17}$$ eV. We use an astrophysical model with two extragalactic source populations to model the hardening of the cosmic-ray flux at around 5 × 10$$^{18}$$ eV (the so-called “ankle” feature) as a transition between these two components. We find our data to be well reproduced if sources above the ankle emit a mixed composition with a hard spectrum and a low rigidity cutoff. The component below the ankle is required to have a very soft spectrum and a mix of protons and intermediate-mass nuclei. The origin of this intermediate-mass component is not well constrained and it could originate from either Galactic or extragalactic sources.To the aim of evaluating our capability to constrain astrophysical models, we discuss the impact on the fit results of the main experimental systematic uncertainties and of the assumptions about quantities affecting the air shower development as well as the propagation and redshift distribution of injected ultra-high-energy cosmic rays (UHECRs).
Research Organization:
ABC Federal U.; ASFYON; Aachen, Tech. Hochsch.; Adelaide U.; Amsterdam U.; Bath U.; Brussels U., IIHE; Bucharest U.; Bucharest, Inst. Space Science; Bucharest, Polytechnic Inst.; Buenos Aires U.; Buenos Aires, CONICET; Buenos Aires, IAFE; CEFET, Rio de Janeiro; CEFIMAS, Buenos Aires; CINVESTAV, IPN; Campinas State U.; Catania U.; Centro Atomico Bariloche; Charles U.; Chiapas Autonoma U.; Chicago U., EFI; Colorado School of Mines; Cracow, INP; Delaware U.; Dortmund U.; Gran Sasso; Granada U.; Hamburg U.; IASF, Palermo; ICAS, UNSAM, Buenos Aires; IFMT, Caceres; IJCLab, Orsay; INFN, Aquila; INFN, Catania; INFN, Lecce; INFN, Milan; INFN, Naples; INFN, Rome2; INFN, Turin; ITeDA, Buenos Aires; KIT, Karlsruhe, ETP; KIT, Karlsruhe, IAP; KIT, Karlsruhe, IPE; L'Aquila U.; LPNHE, Paris; LPSC, Grenoble; La Plata U.; Lehman Coll.; Lisbon, CFTP; Lodz U.; Medellin U.; Messina U.; Mexico U., ICN; Michigan Tech. U.; Milan U.; Milan, Polytech.; NIKHEF, Amsterdam; Naples U.; Natl. Tech. U., San Rafael; New York U. (main); Nijmegen U., IMAPP; Niteroi, Fluminense U.; Nova Gorica U.; OATo, Turin; Palacky U.; Palermo U.; Parana U.; Pierre Auger Observ.; Prague, Inst. Phys.; Puebla U., Inst. Fis.; Rio de Janeiro Federal U.; Rome U., Tor Vergata; Rosario U.; Salento U.; 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; Valongo Observ.; 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:
1915441
Report Number(s):
FERMILAB-PUB-22-876-AD-PPD-SCD-TD; oai:inspirehep.net:2177649; arXiv:2211.02857
Journal Information:
JCAP, Journal Name: JCAP Vol. 05
Country of Publication:
United States
Language:
English

Similar Records

Combined fit of spectrum and composition data as measured by the Pierre Auger Observatory
Journal Article · Sat Apr 01 00:00:00 EDT 2017 · Journal of Cosmology and Astroparticle Physics · OSTI ID:22679904
Combined fit of spectrum and composition data as measured by the Pierre Auger Observatory
Journal Article · Wed Apr 19 20:00:00 EDT 2017 · Journal of Cosmology and Astroparticle Physics · OSTI ID:1343967
Impact of the magnetic horizon on the interpretation of the Pierre Auger Observatory spectrum and composition data
Journal Article · Tue Jul 30 20:00:00 EDT 2024 · JCAP · OSTI ID:2426470

Related Subjects

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