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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Towards Understanding the Origin of Cosmic-Ray Electrons

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Author(s):
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Aguilar, M. [1] ; Cavasonza, L. Ali [2, 3] ; Alpat, B. [4] ; Ambrosi, G. [4] ; Arruda, L. [5] ; Attig, N. [6, 7] ; Azzarello, P. [8] ; Bachlechner, A. [2, 3] ; Barao, F. [5] ; Barrau, A. [9] ; Barrin, L. [10] ; Bartoloni, A. [11] ; Basara, L. [12] ; Basegmez-du Pree, S. [13] ; Battiston, R. [14, 12, 15] ; Becker, U. [16] ; Behlmann, M. [16] ; Beischer, B. [2, 3] ; Berdugo, J. [1] ; Bertucci, B. [17, 4] ; Bindi, V [18] ; de Boer, W. [19] ; Bollweg, K. [20] ; Borgia, B. [21, 11] ; Boschini, M. J. [22] ; Bourquin, M. [8] ; Bueno, E. F. [23] ; Burger, J. [16] ; Burger, W. J. [12] ; Cai, X. D. [16] ; Capell, M. [16] ; Caroff, S. [24] ; Casaus, J. [1] ; Castellini, G. [25] ; Cervelli, F. [26] ; Chang, Y. H. [27, 28] ; Chen, G. M. [29] ; Chen, H. S. [30, 29] ; Chen, Y. [8] ; Cheng, L. [31] ; Chou, H. Y. [27, 28] ; Choutko, V [16] ; Chung, C. H. [2, 3] ; Clark, C. [16, 20] ; Coignet, G. [24] ; Consolandi, C. [18] ; Contin, A. [32, 33] ; Corti, C. [18] ; Crispoltoni, M. [17, 4] ; Cui, Z. [31] ; Dadzie, K. [16] ; Dai, Y. M. [34] ; Datta, A. [18] ; Delgado, C. [1] ; Della Torre, S. [22] ; Demirkoz, M. B. [35] ; Derome, L. [9] ; Di Falco, S. [26] ; Di Felice, V [4, 36] ; Dimiccoli, F. [10, 12] ; Diaz, C. [1] ; von Doetinchem, P. [18] ; Dong, F. [37] ; Donnini, F. [4, 36] ; Duranti, M. [4] ; Egorov, A. [16] ; Eline, A. [16] ; Eronen, T. [38] ; Feng, J. [16] ; Fiandrini, E. [17, 4] ; Fisher, P. [16] ; Formato, V [4] ; Galaktionov, Y. [16] ; Garcia-Lopez, R. J. [39, 40] ; Gargiulo, C. [10] ; Gast, H. [2, 3] ; Gebauer, I [19] ; Gervasi, M. [41, 22] ; Giovacchini, F. [1] ; Gomez-Coral, D. M. [42] ; Gong, J. [37] ; Goy, C. [24] ; Grabski, V [42] ; Grandi, D. [41, 22] ; Graziani, M. [19] ; Guo, K. H. [43] ; Haino, S. [44] ; Han, K. C. [45] ; He, Z. H. [43] ; Heil, M. [16] ; Hsieh, T. H. [16] ; Huang, H. [44, 46] ; Huang, Z. C. [43] ; Incagli, M. [26] ; Jia, Yi [16] ; Jinchi, H. [45] ; Kanishev, K. [12] ; Khiali, B. [4, 36] ; Kirn, Th [2, 3] ; Konak, C. [35] ; Kounin, O. [16] ; Kounine, A. [16] ; Koutsenko, V [16] ; Kulemzin, A. [16] ; La Vacca, G. [41, 22] ; Laudi, E. [10] ; Laurenti, G. [33] ; Lazzizzera, I [12, 15] ; Lebedev, A. [16] ; Lee, H. T. [47] ; Lee, S. C. [44] ; Leluc, C. [8] ; Li, J. Q. [37] ; Li, Q. [37] ; Li, T. X. [43] ; Li, Z. H. [29] ; Light, C. [18] ; Lin, C. H. [44] ; Lipper, T. [6, 7] ; Liu, F. Z. [16] ; Liu, Hu [16, 27, 28] ; Liu, Z. [8] ; Lu, S. Q. [43] ; Lu, Y. S. [29] ; Luebelsmeyer, K. [2, 3] ; Luo, F. [31] ; Luo, J. Z. [37] ; Luo, Xi [18] ; Lyu, S. S. [43] ; Machate, F. [2, 3] ; Mana, C. [1] ; Marin, J. [1] ; Martin, T. [16, 20] ; Martinez, G. [1] ; Masi, N. [33] ; Maurin, D. [9] ; Menchaca-Rocha, A. [42] ; Meng, Q. [37] ; Mo, D. C. [43] ; Molero, M. [1] ; Mott, P. [16, 20] ; Mussolin, L. [17, 4] ; Nelson, T. [18] ; Ni, J. Q. [43] ; Nikonov, N. [2, 3] ; Nozzoli, F. [12] ; Oliva, A. [1] ; Orcinha, M. [5] ; Palermo, M. [18] ; Palmonari, F. [32, 33] ; Paniccia, M. [8] ; Pashnin, A. [16] ; Pauluzzi, M. [17, 4] ; Pensotti, S. [41, 22] ; Perrina, C. [8] ; Phan, H. D. [16] ; Picot-Clemente, N. [48] ; Plyaskin, V [16] ; Pohl, M. [8] ; Poireau, V [24] ; Popkow, A. [18] ; Quadrani, L. [32, 33] ; Qi, X. M. [43] ; Qin, X. [16] ; Qu, Z. Y. [44] ; Rancoita, P. G. [22] ; Rapin, D. [8] ; Reina Conde, A. [39, 40] ; Rosier-Lee, S. [24] ; Rozhkov, A. [16] ; Rozza, D. [41, 22] ; Sagdeev, R. [49] ; Solano, C. [16] ; Schael, S. [2, 3] ; Schmidt, S. M. [6, 7] ; von Dratzig, A. Schulz [2, 3] ; Schwering, G. [2, 3] ; Seo, E. S. [48] ; Shan, B. S. [50] ; Shi, J. Y. [37] ; Siedenburg, T. [2, 3] ; Song, J. W. [31] ; Sun, Z. T. [30, 29] ; Tacconi, M. [41, 22] ; Tang, X. W. [29] ; Tang, Z. C. [29] ; Tian, J. [17, 4] ; Ting, Samuel C. C. [16, 10] ; Ting, S. M. [16] ; Tomassetti, N. [17, 4] ; Torsti, J. [38] ; Urban, T. [16, 20] ; Vagelli, V. [17, 4] ; Valente, E. [21, 11] ; Valtonen, E. [38] ; Vazquez Acosta, M. [39, 40] ; Vecchi, M. [13, 23] ; Velasco, M. [1] ; Vialle, J. P. [24] ; Vizan, J. [1] ; Wang, L. Q. [31] ; Wang, N. H. [31] ; Wang, Q. L. [34] ; Wang, X. [16] ; Wang, X. Q. [30, 29] ; Wang, Z. X. [43] ; Wei, J. [8] ; Weng, Z. L. [16] ; Wu, H. [37] ; Xiong, R. Q. [37] ; Xu, W. [16] ; Yan, Q. [16] ; Yang, Y. [51] ; Yi, H. [37] ; Yu, Y. J. [34] ; Yu, Z. Q. [29] ; Zannoni, M. [41, 22] ; Zeissler, S. [19] ; Zhang, C. [29] ; Zhang, F. [29] ; Zhang, J. H. [37] ; Zhang, Z. [16] ; Zhao, F. [30, 29] ; Zheng, Z. M. [50] ; Zhuang, H. L. [29] ; Zhukov, V [2, 3] ; Zichichi, A. [32, 33] ; Zimmerman, N. [2, 3] ; Zuccon, P. [12, 15] ; Collaboration, AMS
Total Authors: 230
Affiliation:
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[1] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid - Spain
[2] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen - Germany
[3] Rhein Westfal TH Aachen, Phys Inst 1, D-52056 Aachen - Germany
[4] INFN, Sez Perugia, I-06100 Perugia - Italy
[5] Lab Instrumentacao & Fis Expt Particulas LIP, P-1000 Lisbon - Portugal
[6] Res Ctr Julich, JARA FAME, D-52425 Julich - Germany
[7] Julich Supercomp Ctr, D-52425 Julich - Germany
[8] Univ Geneva, DPNC, CH-1211 Geneva 4 - Switzerland
[9] Univ Grenoble Alpes, Grenoble INP, CNRS, LPSC IN2P3, F-38000 Grenoble - France
[10] European Org Nucl Res, CERN, CH-1211 Geneva 23 - Switzerland
[11] INFN, Sez Roma 1, I-00185 Rome - Italy
[12] INFN, TIFPA, I-38123 Trento - Italy
[13] Univ Groningen, KVI Ctr Adv Radiat Technol, NL-9700 AB Groningen - Netherlands
[14] ASI, I-00133 Rome - Italy
[15] Univ Trento, I-38123 Trento - Italy
[16] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 - USA
[17] Univ Perugia, I-06100 Perugia - Italy
[18] Univ Hawaii, Phys & Astron Dept, Honolulu, HI 96822 - USA
[19] Karlsruhe Inst Technol, Inst Expt Teilchenphys, D-76131 Karlsruhe - Germany
[20] NASA, Johnson Space Ctr, Houston, TX 77058 - USA
[21] Univ Roma La Sapienza, I-00185 Rome - Italy
[22] INFN, Sez Milano Bicocca, I-20126 Milan - Italy
[23] Univ Sao Paulo, Inst Fis Sao Carlos, CP 369, BR-13560970 Sao Carlos, SP - Brazil
[24] Univ Grenoble Alpes, Univ Savoie Mont Blanc, CNRS, LAPP IN2P3, F-74000 Annecy - France
[25] CNR, IROE, I-50125 Florence - Italy
[26] INFN, Sez Pisa, I-56100 Pisa - Italy
[27] Natl Cent Univ, Phys Dept, Taoyuan 32054 - Taiwan
[28] Natl Cent Univ, Ctr High Energy & High Field, Taoyuan 32054 - Taiwan
[29] Chinese Acad Sci, IHEP, Beijing 100049 - Peoples R China
[30] Univ Chinese Acad Sci, Beijing 100049 - Peoples R China
[31] Shandong Univ SDU, Jinan 250100, Shandong - Peoples R China
[32] Univ Bologna, I-40126 Bologna - Italy
[33] INFN, Sez Bologna, I-40126 Bologna - Italy
[34] Chinese Acad Sci, IEE, Beijing 100190 - Peoples R China
[35] Middle East Tech Univ, Dept Phys, TR-06800 Ankara - Turkey
[36] ASI Space Sci Data Ctr SSDC, I-00133 Rome - Italy
[37] Southeast Univ SEU, Nanjing 210096, Jiangsu - Peoples R China
[38] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku - Finland
[39] Univ La Laguna, Dept Astrofis, E-38206 Tenerife - Spain
[40] Inst Astrofis Canaries, E-38205 San Cristobal la Laguna - Spain
[41] Univ Milano Bicocca, I-20126 Milan - Italy
[42] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF - Mexico
[43] Sun Yat Sen Univ, Guangzhou 510275, Guangdong - Peoples R China
[44] Acad Sinica, Inst Phys, Taipei 11529 - Taiwan
[45] Natl Chung Shan Inst Sci & Technol, Tao Yuan 32546 - Taiwan
[46] Wuhan Univ, Wuhan 430072, Hubei - Peoples R China
[47] ASGC, Taipei 11529 - Taiwan
[48] Univ Maryland, IPST, College Pk, MD 20742 - USA
[49] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 - USA
[50] Beihang Univ, BUAA, Beijing 100191 - Peoples R China
[51] Natl Cheng Kung Univ, Tainan 70101 - Taiwan
Total Affiliations: 51
Document type: Journal article
Source: Physical Review Letters; v. 122, n. 10 MAR 13 2019.
Web of Science Citations: 6
Abstract

Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1 x 10(6) electrons collected by the Alpha Magnetic Spectrometer on the International Space Station. In the entire energy range the electron and positron spectra have distinctly different magnitudes and energy dependences. The electron flux exhibits a significant excess starting from 42.1(-5.2)(+5.4) GeV compared to the lower energy trends, but the nature of this excess is different from the positron flux excess above 25.2 +/- 1.8 GeV. Contrary to the positron flux, which has an exponential energy cutoff of 810(-180)(+310) GeV, at the 5 sigma level the electron flux does not have an energy cutoff below 1.9 TeV. In the entire energy range the electron flux is well described by the sum of two power law components. The different behavior of the cosmic-ray electrons and positrons measured by the Alpha Magnetic Spectrometer is clear evidence that most high energy electrons originate from different sources than high energy positrons. (AU)

FAPESP's process: 14/19149-7 - Indirect dark matter search with the AMS-02 detector
Grantee:Manuela Vecchi
Support type: Research Grants - Young Investigators Grants