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000622942 0247_ $$2arXiv$$aarXiv:2411.08189
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000622942 088__ $$2arXiv$$aarXiv:2411.08189
000622942 1001_ $$aAharonian, F.$$b0
000622942 245__ $$aHigh-Statistics Measurement of the Cosmic-Ray Electron Spectrum with H.E.S.S.
000622942 260__ $$aCollege Park, Md.$$bAPS$$c2024
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000622942 500__ $$aPhys. Rev. Lett. 133, 221001 (2024). PhysRevLett.133.221001. main paper: 8 pages, 4 figures, supplemental material: 12 pages, 14 figures, accepted for publication in Physical Review Letters https://journals.aps.org/prl/
000622942 520__ $$aOwing to their rapid cooling rate and hence loss-limited propagation distance, cosmic-ray electrons and positrons (CRe) at very high energies probe local cosmic-ray accelerators and provide constraints on exotic production mechanisms such as annihilation of dark matter particles. We present a high-statistics measurement of the spectrum of CRe candidate events from 0.3 to 40 TeV with the High Energy Stereoscopic System, covering 2 orders of magnitude in energy and reaching a proton rejection power of better than 104. The measured spectrum is well described by a broken power law, with a break around 1 TeV, where the spectral index increases from Γ1=3.25±0.02(stat)±0.2(sys) to Γ2=4.49±0.04(stat)±0.2(sys). Apart from the break, the spectrum is featureless. The absence of distinct signatures at multi-TeV energies imposes constraints on the presence of nearby CRe accelerators and the local CRe propagation mechanisms.
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000622942 7001_ $$aAit Benkhali, F.$$b1
000622942 7001_ $$aAschersleben, J.$$b2
000622942 7001_ $$aAshkar, H.$$b3
000622942 7001_ $$aBackes, M.$$b4
000622942 7001_ $$0P:(DE-H253)PIP1085491$$aBarbosa Martins, V.$$b5$$udesy
000622942 7001_ $$aBatzofin, R.$$b6
000622942 7001_ $$aBecherini, Y.$$b7
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000622942 7001_ $$aBernlöhr, K.$$b9
000622942 7001_ $$aBi, B.$$b10
000622942 7001_ $$aBöttcher, M.$$b11
000622942 7001_ $$aBoisson, C.$$b12
000622942 7001_ $$aBolmont, J.$$b13
000622942 7001_ $$ade Bony de Lavergne, M.$$b14
000622942 7001_ $$aBorowska, J.$$b15
000622942 7001_ $$aBouyahiaoui, M.$$b16
000622942 7001_ $$aBrose, R.$$b17
000622942 7001_ $$aBrown, A.$$b18
000622942 7001_ $$aBrun, F.$$b19
000622942 7001_ $$aBruno, B.$$b20
000622942 7001_ $$aBulik, T.$$b21
000622942 7001_ $$aBurger-Scheidlin, C.$$b22
000622942 7001_ $$aBylund, T.$$b23
000622942 7001_ $$aCasanova, S.$$b24
000622942 7001_ $$aCelic, J.$$b25
000622942 7001_ $$aCerruti, M.$$b26
000622942 7001_ $$aChand, T.$$b27
000622942 7001_ $$aChandra, S.$$b28
000622942 7001_ $$aChen, A.$$b29
000622942 7001_ $$aChibueze, J.$$b30
000622942 7001_ $$aChibueze, O.$$b31
000622942 7001_ $$aCollins, T.$$b32
000622942 7001_ $$aCotter, G.$$b33
000622942 7001_ $$0P:(DE-HGF)0$$aDamascene Mbarubucyeye, J.$$b34
000622942 7001_ $$aDevin, J.$$b35
000622942 7001_ $$aDjuvsland, J.$$b36
000622942 7001_ $$aDmytriiev, A.$$b37
000622942 7001_ $$0P:(DE-HGF)0$$aEgberts, K.$$b38$$eCorresponding author
000622942 7001_ $$aEinecke, S.$$b39
000622942 7001_ $$aErnenwein, J.-P.$$b40
000622942 7001_ $$aFegan, S.$$b41
000622942 7001_ $$aFeijen, K.$$b42
000622942 7001_ $$aFontaine, G.$$b43
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000622942 7001_ $$aHuang, Zhiqiu$$b55
000622942 7001_ $$aJamrozy, M.$$b56
000622942 7001_ $$aJankowsky, F.$$b57
000622942 7001_ $$aJoshi, V.$$b58
000622942 7001_ $$aJung-Richardt, I.$$b59
000622942 7001_ $$aKasai, E.$$b60
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000622942 7001_ $$aMarandon, V.$$b81
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000622942 7001_ $$aMartí-Devesa, G.$$b83
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000622942 7001_ $$aSteppa, C.$$b130
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000622942 7001_ $$aVecchi, M.$$b138
000622942 7001_ $$aVenter, C.$$b139
000622942 7001_ $$aVink, J.$$b140
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000622942 7001_ $$aWagner, S. J.$$b142
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000622942 7001_ $$aZech, A.$$b146
000622942 7001_ $$aZywucka, N.$$b147
000622942 7001_ $$aH. E. S. S. Collaboration$$b148$$eCollaboration Author
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