Constraining models for the origin of ultra-high-energy cosmic rays with a novel combined analysis of arrival directions, spectrum, and composition data measured at the Pierre Auger Observatory

被引：0

作者：

Halim, A. Abdul ^{[20
]}

Abreu, P. ^{[78
,79
]}

Aglietta, M. ^{[58
,60
]}

Allekotte, I ^{[1
,2
]}

Cheminant, K. Almeida ^{[76
]}

Almela, A. ^{[13
,19
]}

Aloisio, R. ^{[51
,52
]}

Alvarez-Muniz, J. ^{[87
]}

Ammerman Yebra, J. ^{[87
]}

Anastasi, G. A. ^{[58
,60
]}

Anchordoqui, L. ^{[94
]}

Andrada, B. ^{[13
]}

Andringa, S. ^{[78
,79
]}

Aramo, C. ^{[56
]}

Ferreira, P. R. Araujo ^{[48
]}

Arnone, E. ^{[58
,69
]}

Arteaga Velazquez, J. C. ^{[73
]}

Asorey, H. ^{[13
]}

Assis, P. ^{[78
,79
]}

Avila, G. ^{[17
,18
]}

Avocone, E. ^{[52
,63
]}

Badescu, A. M. ^{[82
]}

Bakalova, A. ^{[39
]}

Balaceanu, A. ^{[80
]}

Barbato, F. ^{[51
,52
]}

Mocellin, A. Bartz ^{[93
]}

Bellido, J. A. ^{[20
,75
]}

Berat, C. ^{[43
]}

Bertaina, M. E. ^{[58
,69
]}

Bhatta, G. ^{[76
]}

Bianciotto, M. ^{[58
,69
]}

Biermann, P. L. ^{[109
]}

Binet, V ^{[9
,10
]}

Bismark, K. ^{[13
,45
]}

Bister, T. ^{[88
,89
]}

Biteau, J. ^{[41
]}

Blazek, J. ^{[39
]}

Bleve, C. ^{[43
]}

Bluemer, J. ^{[47
]}

Bohacova, M. ^{[39
]}

Boncioli, D. ^{[52
,63
]}

Bonifazi, C. ^{[5
,14
,15
,33
]}

Arbeletche, L. Bonneau ^{[28
]}

Borodai, N. ^{[76
]}

Brack, J. ^{[111
]}

Brichetto Orchera, P. G. ^{[13
]}

Briechle, F. L. ^{[48
]}

Bueno, A. ^{[85
,86
]}

Buitink, S. ^{[22
]}

Buscemi, M. ^{[53
,67
]}

机构：

[1] Ctr Mico Bariloche, San Carlos De Bariloche, Rio Negro, Argentina

[2] Inst Balseiro CNEA UNCuyo CONICET, San Carlos De Bariloche, Rio Negro, Argentina

[3] Univ Buenos Aires, Dept Fis, FCEyN, Buenos Aires, DF, Argentina

[4] Univ Buenos Aires, Dept Ciencias Atmosfera & Oceanos, FCEyN, Buenos Aires, DF, Argentina

[5] Consejo Nacl Invest Cient & Tecn, Campus Miguelete San Martin, Buenos Aires, DF, Argentina

[6] Univ Nacl La Plata, IFLP, La Plata, Argentina

[7] Consejo Nacl Invest Cient & Tecn, La Plata, Argentina

[8] CONICET UBA, Inst Astron & Fis Espacio IAFE, Buenos Aires, DF, Argentina

[9] CONICET UNR, Inst Fis Rosario IFIR, Rosario, Santa Fe, Argentina

[10] UNR, Fac Ciencias Bioquim & Farmaceut, Rosario, Santa Fe, Argentina

[11] UNSAM, Inst Tecnol Detecc & Astroparticulas, CONICET, CNEA, Mendoza, Argentina

[12] Univ Tecnol Nacl, Fac Reg Mendoza CONICET CNEA, Mendoza, Argentina

[13] UNSAM, Inst Tecnol Detecc & Astroparticulas, CONICET, CNEA, Buenos Aires, DF, Argentina

[14] Int Ctr Adv Studies, Campus Miguelete San Martin, Buenos Aires, DF, Argentina

[15] ECyT UNSAM, Inst Ciencias Fis, Campus Miguelete San Martin, Buenos Aires, DF, Argentina

[16] UNIDEF CITEDEF CONICET, Lab Atmosfera, Dept Invest Laseres & Sus Aplicac, Buenos Aires, DF, Argentina

[17] Observ Pierre Auger, Malargue, Argentina

[18] Comis Nacl Energia Atom, Malargue, Argentina

[19] Univ Tecnol Nacl, Fac Reg Buenos Aires, Buenos Aires, DF, Argentina

[20] Univ Adelaide, Adelaide, SA, Australia

[21] Univ Libre Bruxelles ULB, Brussels, Belgium

[22] Vrije Univ Brussels, Brussels, Belgium

[23] Ctr Fed Educ Tecnol Celso Suckow da Fonseca, Petropolis, RJ, Brazil

[24] Inst Fed Educ Ciencia & Tecnol Rio de Janeiro IFR, Rio De Janeiro, Brazil

[25] Univ Sao Paulo, Escola Engn Lorena, Lorena, SP, Brazil

[26] Univ Sao Paulo, Inst Fis Sao Carlos, Sao Carlos, SP, Brazil

[27] Univ Sao Paulo, Inst Fis, Sao Paulo, SP, Brazil

[28] Univ Estadual Campinas, IFGW, Campinas, SP, Brazil

[29] Univ Estadual Feira de Santana, Feira De Santana, BA, Brazil

[30] Univ Fed Campina Grande, Ctr Ciencias & Tecnol, Campina Grande, Paraiba, Brazil

[31] Univ Fed ABC, Santo Andre, SP, Brazil

[32] Univ Fed Parana, Setor Palotina, Palotina, Brazil

[33] Univ Fed Rio de Janeiro, Inst Fis, Rio De Janeiro, RJ, Brazil

[34] Univ Fed Rio de Janeiro UFRJ, Observ Valongo, Rio De Janeiro, RJ, Brazil

[35] Univ Fed Fluminense, EEIMVR, Volta Redonda, RJ, Brazil

[36] Univ Medellin, Medellin, Colombia

[37] Univ Ind Santander, Bucaramanga, Colombia

[38] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, Prague, Czech Republic

[39] Czech Acad Sci, Inst Phys, Prague, Czech Republic

[40] Palacky Univ, Olomouc, Czech Republic

[41] Univ Paris Saclay, IJCLab, CNRS IN2P3, Orsay, France

[42] Univ Paris, Sorbonne Univ, Lab Phys Nucl & Hautes Energies LPNHE, CNRS IN2P3, Paris, France

[43] Univ Grenoble Alpes, Grenoble Inst Engn, CNRS, LPSC IN2P3, F-38000 Grenoble, France

[44] Berg Univ Wuppertal, Dept Phys, Wuppertal, Germany

[45] Karlsruhe Inst Technol KIT, Inst Expt Particle Phys, Karlsruhe, Germany

[46] Karlsruhe Inst Technol KIT, Inst Prozessdatenverarbeitung & Elekt, Karlsruhe, Germany

[47] Karlsruhe Inst Technol KIT, Inst Astroparticle Phys, Karlsruhe, Germany

[48] Rhein Westfal TH Aachen, Phys Inst A 3, Aachen, Germany

[49] Univ Hamburg, Inst Theoret Phys 2, Hamburg, Germany

[50] Univ Siegen, Dept Phys Expt Teilchenphys, Siegen, Germany

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2024年 / 01期

基金：

巴西圣保罗研究基金会; 美国国家科学基金会; 澳大利亚研究理事会;

关键词：

ultra high energy cosmic rays; cosmic ray experiments; active galactic nuclei; CONSEQUENCES; PROPAGATION; RADIATION; FRAMEWORK; CENTAURUS; TALYS;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The combined fit of the measured energy spectrum and shower maximum depth distributions of ultra-high-energy cosmic rays is known to constrain the parameters of astrophysical models with homogeneous source distributions. Studies of the distribution of the cosmic-ray arrival directions show a better agreement with models in which a fraction of the flux is non-isotropic and associated with the nearby radio galaxy Centaurus A or with catalogs such as that of starburst galaxies. Here, we present a novel combination of both analyses by a simultaneous fit of arrival directions, energy spectrum, and composition data measured at the Pierre Auger Observatory. The model takes into account a rigidity-dependent magnetic field blurring and an energy-dependent evolution of the catalog contribution shaped by interactions during propagation. We find that a model containing a flux contribution from the starburst galaxy catalog of around 20% at 40 EeV with a magnetic field blurring of around 20. for a rigidity of 10EV provides a fair simultaneous description of all three observables. The starburst galaxy model is favored with a significance of 4.5s (considering experimental systematic effects) compared to a reference model with only homogeneously distributed background sources. By investigating a scenario with Centaurus A as a single source in combination with the homogeneous background, we confirm that this region of the sky provides the dominant contribution to the observed anisotropy signal. Models containing a catalog of jetted active galactic nuclei whose flux scales with the.-ray emission are, however, disfavored as they cannot adequately describe the measured arrival directions.

引用

页数：41

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