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：

Abdul Halim, A. ^{[21
]}

Abreu, P. ^{[80
,81
]}

Aglietta, M. ^{[60
,62
]}

Allekotte, I. ^{[1
,2
]}

Cheminant, K. Almeida ^{[78
]}

Almela, A. ^{[13
,20
]}

Aloisio, R. ^{[53
,54
]}

Alvarez-Muniz, J. ^{[89
]}

Ammerman Yebra, J. ^{[89
]}

Anastasi, G. A. ^{[60
,62
]}

Anchordoqui, L. ^{[96
]}

Andrada, B. ^{[13
]}

Andringa, S. ^{[80
,81
]}

Aramo, C. ^{[58
]}

Ferreira, P. R. Araujo ^{[50
]}

Arnone, E. ^{[60
,71
]}

Arteaga Velazquez, J. C. ^{[75
]}

Asorey, H. ^{[13
]}

Assis, P. ^{[80
,81
]}

Avila, G. ^{[18
,19
]}

Avocone, E. ^{[54
,65
]}

Badescu, A. M. ^{[84
]}

Bakalova, A. ^{[40
]}

Balaceanu, A. ^{[82
]}

Barbato, F. ^{[53
,54
]}

Mocellin, A. Bartz ^{[95
]}

Bellido, J. A. ^{[21
,77
]}

Berat, C. ^{[44
]}

Bertaina, M. E. ^{[60
,71
]}

Bhatta, G. ^{[78
]}

Bianciotto, M. ^{[60
,71
]}

Biermann, P. L. ^{[111
]}

Binet, V. ^{[9
,10
]}

Bismark, K. ^{[13
,47
]}

Bister, T. ^{[90
,91
]}

Biteau, J. ^{[45
]}

Blazek, J. ^{[40
]}

Bleve, C. ^{[44
]}

Bluemer, J. ^{[49
]}

Bohacova, M. ^{[40
]}

Boncioli, D. ^{[54
,65
]}

Bonifazi, C. ^{[14
,15
,16
,34
]}

Bonneau Arbeletche, L. ^{[29
]}

Borodai, N. ^{[78
]}

Brack, J. ^{[113
]}

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

Briechle, F. L. ^{[50
]}

Bueno, A. ^{[87
,88
]}

Buitink, S. ^{[23
]}

Buscemi, M. ^{[55
,69
]}

机构：

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

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

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

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

[5] Consejo Nacl Invest Cient & Tecn, 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] UNR, CONICET, Inst Fis Rosario IFIR, Rosario, Argentina

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

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

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

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

[14] ECyT UNSAM, Int Ctr Adv Studies, Buenos Aires, DF, Argentina

[15] ECyT UNSAM, Inst Ciencias Fis, Buenos Aires, DF, Argentina

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

[17] UNIDEF, CITEDEF CONICET, Lab Atmosfera, Dept Invest Laseres & Aplicaciones, Buenos Aires, DF, Argentina

[18] Observ Pierre Auger, Malargue, Argentina

[19] Comision Nacl Energia Atom, Malargue, Argentina

[20] Uni Tecnol Nacl, Fac Reg Buenos Aires, Buenos Aires, DF, Argentina

[21] Univ Adelaide, Adelaide, SA, Australia

[22] Univ Libre Bruxelles ULB, Brussels, Belgium

[23] Vrije Univ Brussels, Brussels, Belgium

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

[25] Inst Fed Educ Ciencia & Tecnol Rio de Janeiro IFR, Niteroi, RJ, Brazil

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

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

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

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

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

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

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

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

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

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

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

[37] Univ Medellin, Medellin, Colombia

[38] Univ Ind Santander, Bucaramanga, Colombia

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

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

[41] Palacky Univ, Olomouc, Czech Republic

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

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

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

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

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

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

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

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

[50] Rhein Westfal TH Aachen, Phys Inst A 3, Aachen, 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 degrees for a rigidity of 10EV provides a fair simultaneous description of all three observables. The starburst galaxy model is favored with a significance of 4.5 sigma (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 gamma-ray emission are, however, disfavored as they cannot adequately describe the measured arrival directions.

引用

页数：41

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