Direct Measurement of the Spectral Structure of Cosmic-Ray Electrons+Positrons in the TeV Region with CALET on the International Space Station
Creators: name: Adriani, O.
name: Akaike, Y.
name: Asano, K.
name: Asaoka, Y.
name: Berti, E.
name: Bigongiari, G.
name: Binns, W. R.
name: Bongi, M.
name: Brogi, P.
name: Bruno, A.
name: Buckley, J. H.
name: Cannady, N.
name: Castellini, G.
name: Checchia, C.
name: Cherry, M. L.
name: Collazuol, G.
name: de Nolfo, G. A.
name: Ebisawa, K.
name: Ficklin, A. W.
name: Fuke, H.
name: Gonzi, S.
name: Guzik, T. G.
name: Hams, T.
name: Hibino, K.
name: Ichimura, M.
name: Ioka, K.
name: Ishizaki, W.
name: Israel, M. H.
name: Kasahara, K.
name: Kataoka, J.
name: Kataoka, R.
name: Katayose, Y.
name: Kato, C.
name: Kawanaka, N.
name: Kawakubo, Y.
name: Kobayashi, K.
name: Kohri, K.
name: Krawczynski, H. S.
name: Krizmanic, J. F.
name: Maestro, P.
name: Marrocchesi, P. S.
name: Messineo, A. M.
name: Mitchell, J. W.
name: Miyake, S.
name: Moiseev, A. A.
name: Mori, M.
name: Mori, N.
name: Motz, H. M.
name: Munakata, K.
name: Nakahira, S.
name: Nishimura, J.
name: Okuno, S.
name: Ormes, J. F.
name: Ozawa, S.
name: Pacini, L.
name: Papini, P.
name: Rauch, B. F.
name: Ricciarini, S. B.
name: Sakai, K.
name: Sakamoto, 3 T.
name: Sasaki, M.
name: Shimizu, Y.
name: Shiomi, A.
name: Spillantini, P.
name: Stolzi, F.
name: Sugita, S.
name: Sulaj, A.
name: Takita, M.
name: Tamura, T.
name: Terasawa, T.
name: Torii, S.
name: Tsunesada, Y.
name: Uchihori, Y.
name: Vannuccini, E.
name: Wefel, J. P.
name: Yamaoka, K.
name: Yanagita, S.
name: Yoshida, A.
name: Yoshida, K.
name: Zober, W. V.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Detailed measurements of the spectral structure of cosmic-ray electrons and positrons from 10.6 GeV to 7.5 TeV are presented from over 7 years of observations with the CALorimetric Electron Telescope (CALET) on the International Space Station. Because of the excellent energy resolution (a few percent above 10 GeV) and the outstanding e/p separation (10$^5$), CALET provides optimal performance for a detailed search of structures in the energy spectrum. The analysis uses data up to the end of 2022, and the statistics of observed electron candidates has increased more than 3 times since the last publication in 2018. By adopting an updated boosted decision tree analysis, a sufficient proton rejection power up to 7.5 TeV is achieved, with a residual proton contamination less than 10%. The observed energy spectrum becomes gradually harder in the lower energy region from around 30 GeV, consistently with AMS-02, but from 300 to 600 GeV it is considerably softer than the spectra measured by DAMPE and Fermi-LAT. At high energies, the spectrum presents a sharp break around 1 TeV, with a spectral index change from -3.15 to -3.91, and a broken power law fitting the data in the energy range from 30 GeV to 4.8 TeV better than a single power law with 6.9 sigma significance, which is compatible with the DAMPE results. The break is consistent with the expected effects of radiation loss during the propagation from distant sources (except the highest energy bin). We have fitted the spectrum with a model consistent with the positron flux measured by AMS-02 below 1 TeV and interpreted the electron + positron spectrum with possible contributions from pulsars and nearby sources. Above 4.8 TeV, a possible contribution from known nearby supernova remnants, including Vela, is addressed by an event-by-event analysis providing a higher proton-rejection power than a purely statistical analysis.
description: main text: 7 pages, 4 figures; supplemental material: 10 pages, 8 figures, 1 table