Towards Understanding the Origin of Cosmic-Ray Positrons.
M Aguilar, L Ali Cavasonza, G Ambrosi, L Arruda, N Attig, P Azzarello, A Bachlechner, F Barao, A Barrau, L Barrin, A Bartoloni, L Basara, S Başeğmez-du Pree, R Battiston, U Becker, M Behlmann, B Beischer, J Berdugo, B Bertucci, V Bindi, W de Boer, K Bollweg, B Borgia, M J Boschini, M Bourquin, E F Bueno, J Burger, W J Burger, X D Cai, M Capell, S Caroff, J Casaus, G Castellini, F Cervelli, Y H Chang, G M Chen, H S Chen, Y Chen, L Cheng, H Y Chou, V Choutko, C H Chung, C Clark, G Coignet, C Consolandi, A Contin, C Corti, M Crispoltoni, Z Cui, K Dadzie, Y M Dai, A Datta, C Delgado, S Della Torre, M B Demirköz, L Derome, S Di Falco, F Dimiccoli, C Díaz, P von Doetinchem, F Dong, F Donnini, M Duranti, A Egorov, A Eline, T Eronen, J Feng, E Fiandrini, P Fisher, V Formato, Y Galaktionov, R J García-López, C Gargiulo, H Gast, I Gebauer, M Gervasi, F Giovacchini, D M Gómez-Coral, J Gong, C Goy, V Grabski, D Grandi, M Graziani, K H Guo, S Haino, K C Han, Z H He, M Heil, T H Hsieh, H Huang, Z C Huang, M Incagli, Yi Jia, H Jinchi, K Kanishev, B Khiali, Th Kirn, C Konak, O Kounina, A Kounine, V Koutsenko, A Kulemzin, G La Vacca, E Laudi, G Laurenti, I Lazzizzera, A Lebedev, H T Lee, S C Lee, C Leluc, J Q Li, Q Li, T X Li, Z H Li, C Light, C H Lin, T Lippert, F Z Liu, Hu Liu, Z Liu, S Q Lu, Y S Lu, K Luebelsmeyer, F Luo, J Z Luo, Xi Luo, S S Lyu, F Machate, C Mañá, J Marín, T Martin, G Martínez, N Masi, D Maurin, A Menchaca-Rocha, Q Meng, D C Mo, M Molero, P Mott, L Mussolin, T Nelson, J Q Ni, N Nikonov, F Nozzoli, A Oliva, M Orcinha, M Palermo, F Palmonari, M Paniccia, A Pashnin, M Pauluzzi, S Pensotti, C Perrina, H D Phan, N Picot-Clemente, V Plyaskin, M Pohl, V Poireau, A Popkow, L Quadrani, X M Qi, X Qin, Z Y Qu, P G Rancoita, D Rapin, A Reina Conde, S Rosier-Lees, A Rozhkov, D Rozza, R Sagdeev, C Solano, S Schael, S M Schmidt, A Schulz von Dratzig, G Schwering, E S Seo, B S Shan, J Y Shi, T Siedenburg, J W Song, Z T Sun, M Tacconi, X W Tang, Z C Tang, J Tian, Samuel C C Ting, S M Ting, N Tomassetti, J Torsti, T Urban, V Vagelli, E Valente, E Valtonen, M Vázquez Acosta, M Vecchi, M Velasco, J P Vialle, J Vizán, L Q Wang, N H Wang, Q L Wang, X Wang, X Q Wang, Z X Wang, J Wei, Z L Weng, H Wu, R Q Xiong, W Xu, Q Yan, Y Yang, H Yi, Y J Yu, Z Q Yu, M Zannoni, S Zeissler, C Zhang, F Zhang, J H Zhang, Z Zhang, F Zhao, Z M Zheng, H L Zhuang, V Zhukov, A Zichichi, N Zimmermann, P ZucconPrecision 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 4σ. 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.
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