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Towards Understanding the Origin of Cosmic-Ray Electrons

Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1×106 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 magn...

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Detalles Bibliográficos
Autores principales:	Aguilar, M, Ali Cavasonza, L, Alpat, B, Ambrosi, G, Arruda, L, Attig, N, Azzarello, P, Bachlechner, A, Barao, F, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Başeğmez-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, Demirköz, M B, Derome, L, Di Falco, S, Di Felice, V, Dimiccoli, F, Díaz, 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, García-López, R J, Gargiulo, C, Gast, H, Gebauer, I, Gervasi, M, Giovacchini, F, Gómez-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, Mañá, C, Marín, J, Martin, T, Martínez, 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, Conde, A Reina, 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, Acosta, M Vázquez, Vecchi, M, Velasco, M, Vialle, J P, Vizán, 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
Lenguaje:	eng
Publicado:	2019
Materias:	Astrophysics and Astronomy
Acceso en línea:	https://dx.doi.org/10.1103/PhysRevLett.122.101101 http://cds.cern.ch/record/2686972

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author	Aguilar, M Ali Cavasonza, L Alpat, B Ambrosi, G Arruda, L Attig, N Azzarello, P Bachlechner, A Barao, F Barrau, A Barrin, L Bartoloni, A Basara, L Başeğmez-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 Demirköz, M B Derome, L Di Falco, S Di Felice, V Dimiccoli, F Díaz, 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 García-López, R J Gargiulo, C Gast, H Gebauer, I Gervasi, M Giovacchini, F Gómez-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 Mañá, C Marín, J Martin, T Martínez, 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 Conde, A Reina 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 Acosta, M Vázquez Vecchi, M Velasco, M Vialle, J P Vizán, 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
author_facet	Aguilar, M Ali Cavasonza, L Alpat, B Ambrosi, G Arruda, L Attig, N Azzarello, P Bachlechner, A Barao, F Barrau, A Barrin, L Bartoloni, A Basara, L Başeğmez-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 Demirköz, M B Derome, L Di Falco, S Di Felice, V Dimiccoli, F Díaz, 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 García-López, R J Gargiulo, C Gast, H Gebauer, I Gervasi, M Giovacchini, F Gómez-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 Mañá, C Marín, J Martin, T Martínez, 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 Conde, A Reina 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 Acosta, M Vázquez Vecchi, M Velasco, M Vialle, J P Vizán, 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
author_sort	Aguilar, M
collection	CERN
description	Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1×106 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 5σ 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.
id	oai-inspirehep.net-1725636
institution	Organización Europea para la Investigación Nuclear
language	eng
publishDate	2019
record_format	invenio
spelling	oai-inspirehep.net-17256362022-08-10T12:24:44Zdoi:10.1103/PhysRevLett.122.101101http://cds.cern.ch/record/2686972engAguilar, MAli Cavasonza, LAlpat, BAmbrosi, GArruda, LAttig, NAzzarello, PBachlechner, ABarao, FBarrau, ABarrin, LBartoloni, ABasara, LBaşeğmez-du Pree, SBattiston, RBecker, UBehlmann, MBeischer, BBerdugo, JBertucci, BBindi, Vde Boer, WBollweg, KBorgia, BBoschini, M JBourquin, MBueno, E FBurger, JBurger, W JCai, X DCapell, MCaroff, SCasaus, JCastellini, GCervelli, FChang, Y HChen, G MChen, H SChen, YCheng, LChou, H YChoutko, VChung, C HClark, CCoignet, GConsolandi, CContin, ACorti, CCrispoltoni, MCui, ZDadzie, KDai, Y MDatta, ADelgado, CDella Torre, SDemirköz, M BDerome, LDi Falco, SDi Felice, VDimiccoli, FDíaz, Cvon Doetinchem, PDong, FDonnini, FDuranti, MEgorov, AEline, AEronen, TFeng, JFiandrini, EFisher, PFormato, VGalaktionov, YGarcía-López, R JGargiulo, CGast, HGebauer, IGervasi, MGiovacchini, FGómez-Coral, D MGong, JGoy, CGrabski, VGrandi, DGraziani, MGuo, K HHaino, SHan, K CHe, Z HHeil, MHsieh, T HHuang, HHuang, Z CIncagli, MJia, YiJinchi, HKanishev, KKhiali, BKirn, ThKonak, CKounina, OKounine, AKoutsenko, VKulemzin, ALa Vacca, GLaudi, ELaurenti, GLazzizzera, ILebedev, ALee, H TLee, S CLeluc, CLi, J QLi, QLi, T XLi, Z HLight, CLin, C HLippert, TLiu, F ZLiu, HuLiu, ZLu, S QLu, Y SLuebelsmeyer, KLuo, FLuo, J ZLuo, XiLyu, S SMachate, FMañá, CMarín, JMartin, TMartínez, GMasi, NMaurin, DMenchaca-Rocha, AMeng, QMo, D CMolero, MMott, PMussolin, LNelson, TNi, J QNikonov, NNozzoli, FOliva, AOrcinha, MPalermo, MPalmonari, FPaniccia, MPashnin, APauluzzi, MPensotti, SPerrina, CPhan, H DPicot-Clemente, NPlyaskin, VPohl, MPoireau, VPopkow, AQuadrani, LQi, X MQin, XQu, Z YRancoita, P GRapin, DConde, A ReinaRosier-Lees, SRozhkov, ARozza, DSagdeev, RSolano, CSchael, SSchmidt, S Mvon Dratzig, A SchulzSchwering, GSeo, E SShan, B SShi, J YSiedenburg, TSong, J WSun, Z TTacconi, MTang, X WTang, Z CTian, JTing, Samuel C CTing, S MTomassetti, NTorsti, JUrban, TVagelli, VValente, EValtonen, EAcosta, M VázquezVecchi, MVelasco, MVialle, J PVizán, JWang, L QWang, N HWang, Q LWang, XWang, X QWang, Z XWei, JWeng, Z LWu, HXiong, R QXu, WYan, QYang, YYi, HYu, Y JYu, Z QZannoni, MZeissler, SZhang, CZhang, FZhang, J HZhang, ZZhao, FZheng, Z MZhuang, H LZhukov, VZichichi, AZimmermann, NZuccon, PTowards Understanding the Origin of Cosmic-Ray ElectronsAstrophysics and AstronomyPrecision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1×106 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 5σ 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.oai:inspirehep.net:17256362019
spellingShingle	Astrophysics and Astronomy Aguilar, M Ali Cavasonza, L Alpat, B Ambrosi, G Arruda, L Attig, N Azzarello, P Bachlechner, A Barao, F Barrau, A Barrin, L Bartoloni, A Basara, L Başeğmez-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 Demirköz, M B Derome, L Di Falco, S Di Felice, V Dimiccoli, F Díaz, 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 García-López, R J Gargiulo, C Gast, H Gebauer, I Gervasi, M Giovacchini, F Gómez-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 Mañá, C Marín, J Martin, T Martínez, 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 Conde, A Reina 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 Acosta, M Vázquez Vecchi, M Velasco, M Vialle, J P Vizán, 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 Towards Understanding the Origin of Cosmic-Ray Electrons
title	Towards Understanding the Origin of Cosmic-Ray Electrons
title_full	Towards Understanding the Origin of Cosmic-Ray Electrons
title_fullStr	Towards Understanding the Origin of Cosmic-Ray Electrons
title_full_unstemmed	Towards Understanding the Origin of Cosmic-Ray Electrons
title_short	Towards Understanding the Origin of Cosmic-Ray Electrons
title_sort	towards understanding the origin of cosmic-ray electrons
topic	Astrophysics and Astronomy
url	https://dx.doi.org/10.1103/PhysRevLett.122.101101 http://cds.cern.ch/record/2686972
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Towards Understanding the Origin of Cosmic-Ray Electrons

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