Towards Understanding the Origin of Cosmic-Ray Positrons

Aguilar, M.; Cavasonza, L. Ali; Ambrosi, G.; Arruda, L.; Attig, N.; Azzarello, P.; Bachlechner, A.; Barao, F.; Barrau, A.; Barrin, L.; Bartoloni, A.; Basara, L.; Basegmez-du Pree, S.; Battiston, R.; Becker, U.; Behlmann, M.; Beischer, B.; Berdugo, J.; Bertucci, B.; Bindi, V.; de Boer, W.; Bollweg, K.; Borgia, B.; Boschini, M. J.; Bourquin, M.; Bueno, E. F.; Burger, J.; Burger, W. J.; Cai, X. D.; Capell, M.; Caroff, S.; Casaus, J.; Castellini, G.; Cervelli, F.; Chang, Y. H.; Chen, G. M.; Chen, H. S.; Chen, Y.; Cheng, L.; Chou, H. Y.; Choutko, V.; Chung, C. H.; Clark, C.; Coignet, G.; Consolandi, C.; Contin, A.; Corti, C.; Crispoltoni, M.; Cui, Z.; Dadzie, K.; Dai, Y. M.; Datta, A.; Delgado, C.; Della Torre, S.; Demirkoz, M. B.; Derome, L.; Di Falco, S.; Dimiccoli, F.; Diaz, C.; von Doetinchem, P.; Dong, F.; Donnini, F.; Duranti, M.; Egorov, A.; Eline, A.; Eronen, T.; Feng, J.; Fiandrini, E.; Fisher, P.; Formato, V.; Galaktionov, Y.; Garcia-Lopez, R. J.; Gargiulo, C.; Gast, H.; Gebauer, I.; Gervasi, M.; Giovacchini, F.; Gomez-Coral, D. M.; Gong, J.; Goy, C.; Grabski, V.; Grandi, D.; Graziani, M.; Guo, K. H.; Haino, S.; Han, K. C.; He, Z. H.; Heil, M.; Hsieh, T. H.; Huang, H.; Huang, Z. C.; Incagli, M.; Jia, Yi; Jinchi, H.; Kanishev, K.; Khiali, B.; Kirn, Th.; Konak, C.; Kounina, O.; Kounine, A.; Koutsenko, V.; Kulemzin, A.; La Vacca, G.; Laudi, E.; Laurenti, G.; Lazzizzera, I.; Lebedev, A.; Lee, H. T.; Lee, S. C.; Leluc, C.; Li, J. Q.; Li, Q.; Li, T. X.; Li, Z. H.; Light, C.; Lin, C. H.; Lippert, T.; Liu, F. Z.; Liu, Hu; Liu, Z.; Lu, S. Q.; Lu, Y. S.; Luebelsmeyer, K.; Luo, F.; Luo, J. Z.; Luo, Xi; Lyu, S. S.; Machate, F.; Mana, C.; Marin, J.; Martin, T.; Martinez, G.; Masi, N.; Maurin, D.; Menchaca-Rocha, A.; Meng, Q.; Mo, D. C.; Molero, M.; Mott, P.; Mussolin, L.; Nelson, T.; Ni, J. Q.; Nikonov, N.; Nozzoli, F.; Oliva, A.; Orcinha, M.; Palermo, M.; Palmonari, F.; Paniccia, M.; Pashnin, A.; Pauluzzi, M.; Pensotti, S.; Perrina, C.; Phan, H. D.; Picot-Clemente, N.; Plyaskin, V.; Pohl, M.; Poireau, V.; Popkow, A.; Quadrani, L.; Qi, X. M.; Qin, X.; Qu, Z. Y.; Rancoita, P. G.; Rapin, D.; Reina Conde, A.; Rosier-Lees, S.; Rozhkov, A.; Rozza, D.; Sagdeev, R.; Solano, C.; Schael, S.; Schmidt, S. M.; von Dratzig, A. Schulz; Schwering, G.; Seo, E. S.; Shan, B. S.; Shi, J. Y.; Siedenburg, T.; Song, J. W.; Sun, Z. T.; Tacconi, M.; Tang, X. W.; Tang, Z. C.; Tian, J.; Ting, Samuel C. C.; Ting, S. M.; Tomassetti, N.; Torsti, J.; Urban, T.; Vagelli, V.; Valente, E.; Valtonen, E.; Vazquez Acosta, M.; Vecchi, M.; Velasco, M.; Vialle, J. P.; Vizan, J.; Wang, L. Q.; Wang, N. H.; Wang, Q. L.; Wang, X.; Wang, X. Q.; Wang, Z. X.; Wei, J.; Weng, Z. L.; Wu, H.; Xiong, R. Q.; Xu, W.; Yan, Q.; Yang, Y.; Yi, H.; Yu, Y. J.; Yu, Z. Q.; Zannoni, M.; Zeissler, S.; Zhang, C.; Zhang, F.; Zhang, J. H.; Zhang, Z.; Zhao, F.; Zheng, Z. M.; Zhuang, H. L.; Zhukov, V.; Zichichi, A.; Zimmermann, N.; Zuccon, P.; Collaboration, AMS

Texto completo
Autor(es): Mostrar menos -	Aguilar, M. ^[1] ; Cavasonza, L. Ali ^{[2, 3]} ; 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, 21]} ; Borgia, B. ^{[11, 22]} ; Boschini, M. J. ^[23] ; Bourquin, M. ^[8] ; Bueno, E. F. ^[24] ; Burger, J. ^[16] ; Burger, W. J. ^[12] ; Cai, X. D. ^[16] ; Capell, M. ^[16] ; Caroff, S. ^[25] ; Casaus, J. ^[1] ; Castellini, G. ^[26] ; Cervelli, F. ^[27] ; Chang, Y. H. ^{[28, 29]} ; Chen, G. M. ^[30] ; Chen, H. S. ^{[30, 31]} ; Chen, Y. ^[8] ; Cheng, L. ^[32] ; Chou, H. Y. ^{[28, 29]} ; Choutko, V. ^[16] ; Chung, C. H. ^{[2, 3]} ; Clark, C. ^{[20, 21]} ; Coignet, G. ^[25] ; Consolandi, C. ^[18] ; Contin, A. ^{[33, 34]} ; Corti, C. ^[18] ; Crispoltoni, M. ^{[17, 4]} ; Cui, Z. ^[32] ; Dadzie, K. ^[16] ; Dai, Y. M. ^[35] ; Datta, A. ^[18] ; Delgado, C. ^[1] ; Della Torre, S. ^[23] ; Demirkoz, M. B. ^[36] ; Derome, L. ^[9] ; Di Falco, S. ^[27] ; Dimiccoli, F. ^{[10, 12]} ; Diaz, C. ^[1] ; von Doetinchem, P. ^[18] ; Dong, F. ^[37] ; Donnini, F. ^{[4, 38]} ; Duranti, M. ^[4] ; Egorov, A. ^[16] ; Eline, A. ^[16] ; Eronen, T. ^[39] ; Feng, J. ^[16] ; Fiandrini, E. ^{[17, 4]} ; Fisher, P. ^[16] ; Formato, V. ^[4] ; Galaktionov, Y. ^[16] ; Garcia-Lopez, R. J. ^{[40, 41]} ; Gargiulo, C. ^[10] ; Gast, H. ^{[2, 3]} ; Gebauer, I. ^[19] ; Gervasi, M. ^{[23, 42]} ; Giovacchini, F. ^[1] ; Gomez-Coral, D. M. ^[43] ; Gong, J. ^[37] ; Goy, C. ^[25] ; Grabski, V. ^[43] ; Grandi, D. ^{[23, 42]} ; Graziani, M. ^[19] ; Guo, K. H. ^[44] ; Haino, S. ^[45] ; Han, K. C. ^[46] ; He, Z. H. ^[44] ; Heil, M. ^[16] ; Hsieh, T. H. ^[16] ; Huang, H. ^{[45, 47]} ; Huang, Z. C. ^[44] ; Incagli, M. ^[27] ; Jia, Yi ^[16] ; Jinchi, H. ^[46] ; Kanishev, K. ^[12] ; Khiali, B. ^{[4, 38]} ; Kirn, Th. ^{[2, 3]} ; Konak, C. ^[36] ; Kounina, O. ^[16] ; Kounine, A. ^[16] ; Koutsenko, V. ^[16] ; Kulemzin, A. ^[16] ; La Vacca, G. ^{[23, 42]} ; Laudi, E. ^[10] ; Laurenti, G. ^[33] ; Lazzizzera, I. ^{[12, 15]} ; Lebedev, A. ^[16] ; Lee, H. T. ^[48] ; Lee, S. C. ^[45] ; Leluc, C. ^[8] ; Li, J. Q. ^[37] ; Li, Q. ^[37] ; Li, T. X. ^[44] ; Li, Z. H. ^[30] ; Light, C. ^[18] ; Lin, C. H. ^[45] ; Lippert, T. ^{[6, 7]} ; Liu, F. Z. ^[16] ; Liu, Hu ^{[16, 28, 29]} ; Liu, Z. ^[8] ; Lu, S. Q. ^{[44, 45]} ; Lu, Y. S. ^[30] ; Luebelsmeyer, K. ^{[2, 3]} ; Luo, F. ^[32] ; Luo, J. Z. ^[37] ; Luo, Xi ^[18] ; Lyu, S. S. ^[44] ; Machate, F. ^{[2, 3]} ; Mana, C. ^[1] ; Marin, J. ^[1] ; Martin, T. ^{[20, 21]} ; Martinez, G. ^[1] ; Masi, N. ^[33] ; Maurin, D. ^[9] ; Menchaca-Rocha, A. ^[43] ; Meng, Q. ^[37] ; Mo, D. C. ^[44] ; Molero, M. ^[1] ; Mott, P. ^{[20, 21]} ; Mussolin, L. ^{[17, 4]} ; Nelson, T. ^[18] ; Ni, J. Q. ^[44] ; Nikonov, N. ^{[2, 3]} ; Nozzoli, F. ^[12] ; Oliva, A. ^[1] ; Orcinha, M. ^[5] ; Palermo, M. ^[18] ; Palmonari, F. ^{[33, 34]} ; Paniccia, M. ^[8] ; Pashnin, A. ^[16] ; Pauluzzi, M. ^{[17, 4]} ; Pensotti, S. ^{[23, 42]} ; Perrina, C. ^[8] ; Phan, H. D. ^[16] ; Picot-Clemente, N. ^[49] ; Plyaskin, V. ^[16] ; Pohl, M. ^[8] ; Poireau, V. ^[25] ; Popkow, A. ^[18] ; Quadrani, L. ^{[33, 34]} ; Qi, X. M. ^[44] ; Qin, X. ^[16] ; Qu, Z. Y. ^{[45, 50]} ; Rancoita, P. G. ^[23] ; Rapin, D. ^[8] ; Reina Conde, A. ^{[40, 41]} ; Rosier-Lees, S. ^[25] ; Rozhkov, A. ^[16] ; Rozza, D. ^{[23, 42]} ; Sagdeev, R. ^[51] ; 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. ^[49] ; Shan, B. S. ^[52] ; Shi, J. Y. ^[37] ; Siedenburg, T. ^{[2, 3]} ; Song, J. W. ^[32] ; Sun, Z. T. ^[30] ; Tacconi, M. ^{[23, 42]} ; Tang, X. W. ^[30] ; Tang, Z. C. ^[30] ; Tian, J. ^{[17, 4]} ; Ting, Samuel C. C. ^{[10, 16]} ; Ting, S. M. ^[16] ; Tomassetti, N. ^{[17, 4]} ; Torsti, J. ^[39] ; Urban, T. ^{[20, 21]} ; Vagelli, V. ^{[17, 4]} ; Valente, E. ^{[11, 22]} ; Valtonen, E. ^[39] ; Vazquez Acosta, M. ^{[40, 41]} ; Vecchi, M. ^{[13, 24]} ; Velasco, M. ^[1] ; Vialle, J. P. ^[25] ; Vizan, J. ^[1] ; Wang, L. Q. ^[32] ; Wang, N. H. ^[32] ; Wang, Q. L. ^[35] ; Wang, X. ^[16] ; Wang, X. Q. ^{[30, 31]} ; Wang, Z. X. ^[44] ; Wei, J. ^[8] ; Weng, Z. L. ^[16] ; Wu, H. ^[37] ; Xiong, R. Q. ^[37] ; Xu, W. ^[16] ; Yan, Q. ^[16] ; Yang, Y. ^[53] ; Yi, H. ^[37] ; Yu, Y. J. ^[35] ; Yu, Z. Q. ^[30] ; Zannoni, M. ^{[23, 42]} ; Zeissler, S. ^[19] ; Zhang, C. ^[30] ; Zhang, F. ^[30] ; Zhang, J. H. ^[37] ; Zhang, Z. ^[16] ; Zhao, F. ^{[30, 31]} ; Zheng, Z. M. ^[52] ; Zhuang, H. L. ^[30] ; Zhukov, V. ^{[2, 3]} ; Zichichi, A. ^{[33, 34]} ; Zimmermann, N. ^{[2, 3]} ; Zuccon, P. ^{[12, 15]} ; Collaboration, AMS Número total de Autores: 228
Afiliação do(s) autor(es): Mostrar menos -	^[1] Ctr Invest Energet Med Medioambientales & Tecnol, E-28040 Madrid - Spain ^[2] Rhein Westfal TH Aachen, Inst Phys 1, D-52056 Aachen - Germany ^[3] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen - Germany ^[4] Ist Nazl Fis Nucl, 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] Res Ctr Julich, Julich Supercomp Ctr, D-52425 Julich - Germany ^[8] Univ Geneva, DPNC, CH-1211 Geneva 4 - Switzerland ^[9] Univ Grenoble Alpes, CNRS, Grenoble INP, LPSC, IN2P3, F-38000 Grenoble - France ^[10] CERN, European Org Nucl Res, CH-1211 Geneva 23 - Switzerland ^[11] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome - Italy ^[12] Ist Nazl Fis Nucl, TIFPA, I-38123 Povo, 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 Povo, Trento - Italy ^[16] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 - USA ^[17] Univ Perugia, I-06100 Perugia - Italy ^[18] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 - USA ^[19] Karlsruhe Inst Technol, Inst Expt Teilchenphys, D-76131 Karlsruhe - Germany ^[20] Jacobs Engn, Johnson Space Ctr, Natl Aeronaut & Space Adm, Houston, TX 77058 - USA ^[21] Business Integra, Houston, TX 77058 - USA ^[22] Univ Roma La Sapienza, I-00185 Rome - Italy ^[23] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan - Italy ^[24] Univ Sao Paulo, Inst Fis Sao Carlos, CP 369, BR-13560970 Sao Paulo, SP - Brazil ^[25] Univ Savoie Mt Blanc, Univ Grenoble Alpes, CNRS, LAPP, IN2P3, F-74000 Annecy - France ^[26] CNR, IROE, I-50125 Florence - Italy ^[27] Ist Nazl Fis Nucl, Sez Pisa, I-56100 Pisa - Italy ^[28] Natl Cent Univ, Phys Dept, Tao Yuan 32054 - Taiwan ^[29] Natl Cent Univ, Ctr High Energy & High Field, Tao Yuan 32054 - Taiwan ^[30] Chinese Acad Sci, Inst High Energy Phys, Beijing 100049 - Peoples R China ^[31] Univ Chinese Acad Sci, Beijing 100049 - Peoples R China ^[32] Shandong Univ SDU, Jinan 250100, Shandong - Peoples R China ^[33] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna - Italy ^[34] Univ Bologna, I-40126 Bologna - Italy ^[35] Chinese Acad Sci, Inst Elect Engn, Beijing 100190 - Peoples R China ^[36] Middle East Tech Univ, Dept Phys, TR-06800 Ankara - Turkey ^[37] Southeast Univ SEU, Nanjing 210096, Jiangsu - Peoples R China ^[38] ASI, Space Sci Data Ctr, I-00133 Rome - Italy ^[39] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku - Finland ^[40] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna - Spain ^[41] Univ La Laguna, Dept Astrofis, E-38206 Tenerife - Spain ^[42] Univ Milano Bicocca, I-20126 Milan - Italy ^[43] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF - Mexico ^[44] Sun Yat Sen Univ, Guangzhou 510275, Guangdong - Peoples R China ^[45] Acad Sinica, Inst Phys, Taipei 11529 - Taiwan ^[46] NCSIST, Longtan 32546, Tao Yuan - Taiwan ^[47] Wuhan Univ, Wuhan 430072, Hubei - Peoples R China ^[48] Acad Sinica, Grid Ctr, Taipei 11529 - Taiwan ^[49] Univ Maryland, IPST, College Pk, MD 20742 - USA ^[50] Nankai Univ, Tianjin 300071 - Peoples R China ^[51] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 - USA ^[52] Beihang Univ BUAA, Beijing 100191 - Peoples R China ^[53] Natl Cheng Kung Univ, Tainan 70101 - Taiwan Número total de Afiliações: 53
Tipo de documento:	Artigo Científico
Fonte:	Physical Review Letters; v. 122, n. 4 JAN 29 2019.
Citações Web of Science:	17
Resumo
Precision measurements of cosmic ray positrons are presented up to 1 TeV based on 1.9 million positrons collected by the Alpha Magnetic Spectrometer on the International Space Station. The positron flux exhibits complex energy dependence. Its distinctive properties are (a) a significant excess starting from 25.2 +/- 1.8 GeV compared to the lower-energy, power-law trend, (b) a sharp dropoff above 284(-64)(+91) GeV, (c) in the entire energy range the positron flux is well described by the sum of a term associated with the positrons produced in the collision of cosmic rays, which dominates at low energies, and a new source term of positrons, which dominates at high energies, and (d) a finite energy cutoff of the source term of E-s = 810(-180)(+310) GeV is established with a significance of more than 4 sigma. These experimental data on cosmic ray positrons show that, at high energies, they predominantly originate either from dark matter annihilation or from other astrophysical sources. (AU)

Processo FAPESP:	14/19149-7 - Busca indireta de matéria escura com o detector AMS-02
Beneficiário:	Manuela Vecchi
Modalidade de apoio:	Auxílio à Pesquisa - Jovens Pesquisadores

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