1
|
Adriani O, Akaike Y, Asano K, Asaoka Y, Berti E, Bigongiari G, Binns WR, Bongi M, Brogi P, Bruno A, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, de Nolfo GA, Ebisawa K, Ficklin AW, Fuke H, Gonzi S, Guzik TG, Hams T, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kobayashi K, Kohri K, Krawczynski HS, Krizmanic JF, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori M, Mori N, Motz HM, Munakata K, Nakahira S, Nishimura J, Okuno S, Ormes JF, Ozawa S, Pacini L, Papini P, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Spillantini P, Stolzi F, Sugita S, Sulaj A, Takita M, Tamura T, Terasawa T, Torii S, Tsunesada Y, Uchihori Y, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K, Zober WV. Direct Measurement of the Spectral Structure of Cosmic-Ray Electrons+Positrons in the TeV Region with CALET on the International Space Station. PHYSICAL REVIEW LETTERS 2023; 131:191001. [PMID: 38000434 DOI: 10.1103/physrevlett.131.191001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/02/2023] [Revised: 07/31/2023] [Accepted: 10/09/2023] [Indexed: 11/26/2023]
Abstract
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. The instrument, consisting of a charge detector, an imaging calorimeter, and a total absorption calorimeter with a total depth of 30 radiation lengths at normal incidence and a fine shower imaging capability, is optimized to measure the all-electron spectrum well into the TeV region. 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.
Collapse
Affiliation(s)
- O Adriani
- Department of Physics, University of Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
| | - Y Akaike
- Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - E Berti
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019, Sesto Fiorentino, Italy
| | - G Bigongiari
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - W R Binns
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - M Bongi
- Department of Physics, University of Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
| | - P Brogi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A Bruno
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - J H Buckley
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - G Castellini
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019, Sesto Fiorentino, Italy
| | - C Checchia
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - M L Cherry
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Collazuol
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - G A de Nolfo
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - A W Ficklin
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Gonzi
- Department of Physics, University of Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019, Sesto Fiorentino, Italy
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
| | - K Hibino
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - M Ichimura
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - K Ioka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan
| | - W Ishizaki
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - M H Israel
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - K Kasahara
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| | - J Kataoka
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - R Kataoka
- National Institute of Polar Research, 10-3, Midori-cho, Tachikawa, Tokyo 190-8518, Japan
| | - Y Katayose
- Faculty of Engineering, Division of Intelligent Systems Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - C Kato
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - N Kawanaka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan
| | - Y Kawakubo
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Kobayashi
- Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - K Kohri
- Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki, 305-0801, Japan
| | - H S Krawczynski
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - P Maestro
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P S Marrocchesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A M Messineo
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
- University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J W Mitchell
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Miyake
- Department of Electrical and Electronic Systems Engineering, National Institute of Technology (KOSEN), Ibaraki College, 866 Nakane, Hitachinaka, Ibaraki 312-8508, Japan
| | - A A Moiseev
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - M Mori
- Department of Physical Sciences, College of Science and Engineering, Ritsumeikan University, Shiga 525-8577, Japan
| | - N Mori
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
| | - H M Motz
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - K Munakata
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - S Nakahira
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - J Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Okuno
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - J F Ormes
- Department of Physics and Astronomy, University of Denver, Physics Building, Room 211, 2112 East Wesley Avenue, Denver, Colorado 80208-6900, USA
| | - S Ozawa
- Quantum ICT Advanced Development Center, National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan
| | - L Pacini
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019, Sesto Fiorentino, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
| | - B F Rauch
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S B Ricciarini
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019, Sesto Fiorentino, Italy
| | - K Sakai
- Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Sakamoto
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - M Sasaki
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - Y Shimizu
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - A Shiomi
- College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino, Chiba 275-8575, Japan
| | - P Spillantini
- Department of Physics, University of Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
| | - F Stolzi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - S Sugita
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - A Sulaj
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - M Takita
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - T Tamura
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - S Torii
- Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan
| | - Y Tsunesada
- Graduate School of Science, Osaka Metropolitan University, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
- Nambu Yoichiro Institute for Theoretical and Experimental Physics, Osaka Metropolitan University, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
| | - Y Uchihori
- National Institutes for Quantum and Radiation Science and Technology, 4-9-1 Anagawa, Inage, Chiba 263-8555, Japan
| | - E Vannuccini
- INFN Sezione di Florence, Via Sansone, 1-50019, Sesto Fiorentino, Italy
| | - J P Wefel
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Yamaoka
- Nagoya University, Furo, Chikusa, Nagoya 464-8601, Japan
| | - S Yanagita
- College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
| | - A Yoshida
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Yoshida
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| | - W V Zober
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| |
Collapse
|
2
|
Lin YH, Wu WH, Wu MR, Wong HTK. Searching for Afterglow: Light Dark Matter Boosted by Supernova Neutrinos. PHYSICAL REVIEW LETTERS 2023; 130:111002. [PMID: 37001110 DOI: 10.1103/physrevlett.130.111002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/16/2022] [Revised: 11/16/2022] [Accepted: 02/24/2023] [Indexed: 06/19/2023]
Abstract
A novel analysis is performed, incorporating time-of-flight (TOF) information to study the interactions of dark matter (DM) with standard model particles. After supernova (SN) explosions, DM with mass m_{χ}≲O(MeV) in the halo can be boosted by SN neutrinos (SNν) to relativistic speed. The SNν boosted DM (BDM) arrives on Earth with TOF which depends only on m_{χ} and is independent of the cross section. These BDMs can interact with detector targets in low-background experiments and manifest as afterglow events after the arrival of SNν. The characteristic TOF spectra of the BDM events can lead to large background suppression and unique determination of m_{χ}. New cross section constraints on sqrt[σ_{χe}σ_{χν}] are derived from SN1987a in the Large Magellanic Cloud with data from the Kamiokande and Super-Kamiokande experiments. Potential sensitivities for the next galactic SN with Hyper-Kamiokande are projected. This analysis extends the existing bounds on sqrt[σ_{χe}σ_{χν}] over a broad range of r_{χ}=σ_{χν}/σ_{χe}. In particular, the improvement is by 1-3 orders of magnitude for m_{χ}<O(100 keV) for σ_{χe}∼σ_{χν}. Prospects of exploiting TOF information in other astrophysical systems to probe exotic physics with other DM candidates are discussed.
Collapse
Affiliation(s)
- Yen-Hsun Lin
- Institute of Physics, Academia Sinica, Taipei 115, Taiwan
- Physics Division, National Center for Theoretical Sciences, Taipei 106, Taiwan
| | - Wen-Hua Wu
- Institute of Physics, Academia Sinica, Taipei 115, Taiwan
- Department of Physics, National Taiwan University, Taipei 106, Taiwan
| | - Meng-Ru Wu
- Institute of Physics, Academia Sinica, Taipei 115, Taiwan
- Institute of Astronomy and Astrophysics, Academia Sinica, Taipei 106, Taiwan
- Physics Division, National Center for Theoretical Sciences, Taipei 106, Taiwan
| | | |
Collapse
|
3
|
Zhu CR, Cui MY, Xia ZQ, Yu ZH, Huang X, Yuan Q, Fan YZ. Explaining the GeV Antiproton Excess, GeV γ-Ray Excess, and W-Boson Mass Anomaly in an Inert Two Higgs Doublet Model. PHYSICAL REVIEW LETTERS 2022; 129:231101. [PMID: 36563204 DOI: 10.1103/physrevlett.129.231101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/15/2022] [Revised: 09/20/2022] [Accepted: 10/31/2022] [Indexed: 06/17/2023]
Abstract
For the newly discovered W-boson mass anomaly, one of the simplest dark matter (DM) models that can account for the anomaly without violating other astrophysical and experimental constraints is the inert two Higgs doublet model, in which the DM mass (m_{S}) is found to be within ∼54-74 GeV. In this model, the annihilation of DM via SS→bb[over ¯] and SS→WW^{*} would produce antiprotons and gamma rays, and may account for the excesses identified previously in both particles. Motivated by this, we reanalyze the AMS-02 antiproton and Fermi-LAT Galactic center γ-ray data. For the antiproton analysis, the novel treatment is the inclusion of the charge-sign-dependent three-dimensional solar modulation model as constrained by the time-dependent proton data. We find that the excess of antiprotons is more distinct than previous results based on the force-field solar modulation model. The interpretation of this excess as the annihilation of SS→WW^{*} (SS→bb[over ¯]) requires a DM mass of ∼40-80 (40-60) GeV and a velocity-averaged cross section of O(10^{-26}) cm^{3} s^{-1}. As for the γ-ray data analysis, besides adopting the widely used spatial template fitting, we employ an orthogonal approach with a data-driven spectral template analysis. The fitting to the GeV γ-ray excess yields DM model parameters overlapped with those to fit the antiproton excess via the WW^{*} channel. The consistency of the DM particle properties required to account for the W-boson mass anomaly, the GeV antiproton excess, and the GeV γ-ray excess suggests a common origin of them.
Collapse
Affiliation(s)
- Cheng-Rui Zhu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- Shandong Institute of Advanced Technology, Jinan 250100, China
| | - Ming-Yang Cui
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Zi-Qing Xia
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Zhao-Huan Yu
- School of Physics, Sun Yat-Sen University, Guangzhou 510275, China
| | - Xiaoyuan Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, Anhui, China
| | - Qiang Yuan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, Anhui, China
| | - Yi-Zhong Fan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, Anhui, China
| |
Collapse
|
4
|
Detection of spectral hardenings in cosmic-ray boron-to-carbon and boron-to-oxygen flux ratios with DAMPE. Sci Bull (Beijing) 2022; 67:2162-2166. [DOI: 10.1016/j.scib.2022.10.002] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/13/2022] [Revised: 09/09/2022] [Accepted: 09/27/2022] [Indexed: 11/07/2022]
|
5
|
Cholis I, McKinnon I. Constraining the charge-, time-, and rigidity-dependence of cosmic-ray solar modulation with AMS-02 observations during Solar Cycle 24. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.063021] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
6
|
Rankin JS, Bindi V, Bykov AM, Cummings AC, Della Torre S, Florinski V, Heber B, Potgieter MS, Stone EC, Zhang M. Galactic Cosmic Rays Throughout the Heliosphere and in the Very Local Interstellar Medium. SPACE SCIENCE REVIEWS 2022; 218:42. [PMID: 35855211 PMCID: PMC9287243 DOI: 10.1007/s11214-022-00912-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/05/2022] [Accepted: 06/15/2022] [Indexed: 06/15/2023]
Abstract
We review recent observations and modeling developments on the subject of galactic cosmic rays through the heliosphere and in the Very Local Interstellar Medium, emphasizing knowledge that has accumulated over the past decade. We begin by highlighting key measurements of cosmic-ray spectra by Voyager, PAMELA, and AMS and discuss advances in global models of solar modulation. Next, we survey recent works related to large-scale, long-term spatial and temporal variations of cosmic rays in different regimes of the solar wind. Then we highlight new discoveries from beyond the heliopause and link these to the short-term evolution of transients caused by solar activity. Lastly, we visit new results that yield interesting insights from a broader astrophysical perspective.
Collapse
Affiliation(s)
- Jamie S. Rankin
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 USA
| | - Veronica Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, HI 96822 USA
| | | | | | | | - Vladimir Florinski
- Center for Space Plasma and Aeronomic Research (CSPAR) and Department of Space Science, University of Alabama in Huntsville, Huntsville, AL 35805 USA
| | - Bernd Heber
- Institute for Experimental and Applied Physics, Christian Albrechts University in Kiel, Kiel, Germany
| | - Marius S. Potgieter
- Institute for Experimental and Applied Physics, Christian Albrechts University in Kiel, Kiel, Germany
| | | | - Ming Zhang
- Department of Physics and Space Sciences, Florida Institute of Technology, Melbourn, FL 32901 USA
| |
Collapse
|
7
|
Chan MH, Lee CM. Constraints on annihilating dark matter in the Omega Centauri cluster. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.123006] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
8
|
Guo Y, Wu J, Ma H, Wang S, Huang J. Deep Ensemble Learning with Atrous Spatial Pyramid Networks for Protein Secondary Structure Prediction. Biomolecules 2022; 12:biom12060774. [PMID: 35740899 PMCID: PMC9221033 DOI: 10.3390/biom12060774] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/02/2022] [Revised: 05/26/2022] [Accepted: 05/30/2022] [Indexed: 02/04/2023] Open
Abstract
The secondary structure of proteins is significant for studying the three-dimensional structure and functions of proteins. Several models from image understanding and natural language modeling have been successfully adapted in the protein sequence study area, such as Long Short-term Memory (LSTM) network and Convolutional Neural Network (CNN). Recently, Gated Convolutional Neural Network (GCNN) has been proposed for natural language processing. It has achieved high levels of sentence scoring, as well as reduced the latency. Conditionally Parameterized Convolution (CondConv) is another novel study which has gained great success in the image processing area. Compared with vanilla CNN, CondConv uses extra sample-dependant modules to conditionally adjust the convolutional network. In this paper, we propose a novel Conditionally Parameterized Convolutional network (CondGCNN) which utilizes the power of both CondConv and GCNN. CondGCNN leverages an ensemble encoder to combine the capabilities of both LSTM and CondGCNN to encode protein sequences by better capturing protein sequential features. In addition, we explore the similarity between the secondary structure prediction problem and the image segmentation problem, and propose an ASP network (Atrous Spatial Pyramid Pooling (ASPP) based network) to capture fine boundary details in secondary structure. Extensive experiments show that the proposed method can achieve higher performance on protein secondary structure prediction task than existing methods on CB513, Casp11, CASP12, CASP13, and CASP14 datasets. We also conducted ablation studies over each component to verify the effectiveness. Our method is expected to be useful for any protein related prediction tasks, which is not limited to protein secondary structure prediction.
Collapse
Affiliation(s)
- Yuzhi Guo
- Department of Computer Science and Engineering, University of Texas at Arlington, Arlington, TX 76019, USA; (Y.G.); (H.M.); (S.W.)
| | | | - Hehuan Ma
- Department of Computer Science and Engineering, University of Texas at Arlington, Arlington, TX 76019, USA; (Y.G.); (H.M.); (S.W.)
| | - Sheng Wang
- Department of Computer Science and Engineering, University of Texas at Arlington, Arlington, TX 76019, USA; (Y.G.); (H.M.); (S.W.)
| | - Junzhou Huang
- Department of Computer Science and Engineering, University of Texas at Arlington, Arlington, TX 76019, USA; (Y.G.); (H.M.); (S.W.)
- Correspondence:
| |
Collapse
|
9
|
Cholis I, Krommydas I. Utilizing cosmic-ray positron and electron observations to probe the averaged properties of Milky Way pulsars. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.023015] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
10
|
Zhang PP, Qiao BQ, Yuan Q, Cui SW, Guo YQ. Ultrahigh-energy diffuse gamma-ray emission from cosmic-ray interactions with the medium surrounding acceleration sources. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.023002] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
11
|
Lin Z, Lv S, Yang Z, Qiu J, Zhou S. Structured Scintillators for Efficient Radiation Detection. ADVANCED SCIENCE (WEINHEIM, BADEN-WURTTEMBERG, GERMANY) 2022; 9:e2102439. [PMID: 34761546 PMCID: PMC8805559 DOI: 10.1002/advs.202102439] [Citation(s) in RCA: 24] [Impact Index Per Article: 12.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/10/2021] [Revised: 10/04/2021] [Indexed: 05/02/2023]
Abstract
Scintillators, which can convert high-energy ionizing radiation into visible light, have been serving as the core component in radiation detectors for more than a century of history. To address the increasing application demands along with the concern on nuclear security, various strategies have been proposed to develop a next-generation scintillator with a high performance in past decades, among which the novel approach via structure control has received great interest recently due to its high feasibility and efficiency. Herein, the concept of "structure engineering" is proposed for the exploration of this type of scintillators. Via internal or external structure design with size ranging from micro size to macro size, this promising strategy cannot only improve scintillator performance, typically radiation stopping power and light yield, but also extend its functionality for specific applications such as radiation imaging and therapy, opening up a new range of material candidates. The research and development of various types of structured scintillators are reviewed. The current state-of-the-art progresses on structure design, fabrication techniques, and the corresponding applications are discussed. Furthermore, an outlook focusing on the current challenges and future development is proposed.
Collapse
Affiliation(s)
- Ziyu Lin
- State Key Laboratory of Luminescent Materials and DevicesSchool of Materials Science and EngineeringSouth China University of TechnologyGuangdong Provincial Key Laboratory of Fiber Laser Materials and Applied TechniquesGuangdong Engineering Technology Research and Development Center of Special Optical Fiber Materials and DevicesGuangzhou510640China
| | - Shichao Lv
- State Key Laboratory of Luminescent Materials and DevicesSchool of Materials Science and EngineeringSouth China University of TechnologyGuangdong Provincial Key Laboratory of Fiber Laser Materials and Applied TechniquesGuangdong Engineering Technology Research and Development Center of Special Optical Fiber Materials and DevicesGuangzhou510640China
| | - Zhongmin Yang
- State Key Laboratory of Luminescent Materials and DevicesSchool of Materials Science and EngineeringSouth China University of TechnologyGuangdong Provincial Key Laboratory of Fiber Laser Materials and Applied TechniquesGuangdong Engineering Technology Research and Development Center of Special Optical Fiber Materials and DevicesGuangzhou510640China
| | - Jianrong Qiu
- College of Optical Science and EngineeringZhejiang UniversityHangzhou310027China
| | - Shifeng Zhou
- State Key Laboratory of Luminescent Materials and DevicesSchool of Materials Science and EngineeringSouth China University of TechnologyGuangdong Provincial Key Laboratory of Fiber Laser Materials and Applied TechniquesGuangdong Engineering Technology Research and Development Center of Special Optical Fiber Materials and DevicesGuangzhou510640China
| |
Collapse
|
12
|
Fornieri O, Gaggero D, Guberman D, Brahimi L, Luque PDLT, Marcowith A. Diffusive origin for the cosmic-ray spectral hardening reveals signatures of a nearby source in the leptons and protons data. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.103013] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
13
|
Chan MH. Constraining the axion-photon coupling using radio data of the Bullet cluster. Sci Rep 2021; 11:20087. [PMID: 34635710 PMCID: PMC8505521 DOI: 10.1038/s41598-021-99495-3] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/09/2021] [Accepted: 09/21/2021] [Indexed: 11/09/2022] Open
Abstract
Axion is one of the most popular candidates of the cosmological dark matter. Recent studies considering the misalignment production of axions suggest some benchmark axion mass ranges near [Formula: see text] μeV. For such axion mass, the spontaneous decay of axions can give photons in radio band frequency [Formula: see text] GHz, which can be detected by radio telescopes. In this article, we show that using radio data of galaxy clusters would be excellent to constrain axion dark matter. Specifically, by using radio data of the Bullet cluster (1E 0657-55.8), we find that the upper limit of the axion-photon coupling constant can be constrained to [Formula: see text] GeV[Formula: see text] for [Formula: see text] μeV, which is tighter than the limit obtained by the CERN Axion Solar Telescope (CAST).
Collapse
Affiliation(s)
- Man Ho Chan
- Department of Science and Environmental Studies, The Education University of Hong Kong, Tai Po, Hong Kong, New Territories, China.
| |
Collapse
|
14
|
Alemanno F, An Q, Azzarello P, Barbato FCT, Bernardini P, Bi XJ, Cai MS, Catanzani E, Chang J, Chen DY, Chen JL, Chen ZF, Cui MY, Cui TS, Cui YX, Dai HT, D'Amone A, De Benedittis A, De Mitri I, de Palma F, Deliyergiyev M, Di Santo M, Dong TK, Dong ZX, Donvito G, Droz D, Duan JL, Duan KK, D'Urso D, Fan RR, Fan YZ, Fang K, Fang F, Feng CQ, Feng L, Fusco P, Gao M, Gargano F, Gong K, Gong YZ, Guo DY, Guo JH, Guo XL, Han SX, Hu YM, Huang GS, Huang XY, Huang YY, Ionica M, Jiang W, Kong J, Kotenko A, Kyratzis D, Lei SJ, Li S, Li WL, Li X, Li XQ, Liang YM, Liu CM, Liu H, Liu J, Liu SB, Liu WQ, Liu Y, Loparco F, Luo CN, Ma M, Ma PX, Ma T, Ma XY, Marsella G, Mazziotta MN, Mo D, Niu XY, Pan X, Parenti A, Peng WX, Peng XY, Perrina C, Qiao R, Rao JN, Ruina A, Salinas MM, Shang GZ, Shen WH, Shen ZQ, Shen ZT, Silveri L, Song JX, Stolpovskiy M, Su H, Su M, Sun ZY, Surdo A, Teng XJ, Tykhonov A, Wang H, Wang JZ, Wang LG, Wang S, Wang XL, Wang Y, Wang YF, Wang YZ, Wang ZM, Wei DM, Wei JJ, Wei YF, Wen SC, Wu D, Wu J, Wu LB, Wu SS, Wu X, Xia ZQ, Xu HT, Xu ZH, Xu ZL, Xu ZZ, Xue GF, Yang HB, Yang P, Yang YQ, Yao HJ, Yu YH, Yuan GW, Yuan Q, Yue C, Zang JJ, Zhang F, Zhang SX, Zhang WZ, Zhang Y, Zhang YJ, Zhang YL, Zhang YP, Zhang YQ, Zhang Z, Zhang ZY, Zhao C, Zhao HY, Zhao XF, Zhou CY, Zhu Y. Measurement of the Cosmic Ray Helium Energy Spectrum from 70 GeV to 80 TeV with the DAMPE Space Mission. PHYSICAL REVIEW LETTERS 2021; 126:201102. [PMID: 34110215 DOI: 10.1103/physrevlett.126.201102] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/05/2021] [Revised: 03/25/2021] [Accepted: 04/06/2021] [Indexed: 06/12/2023]
Abstract
The measurement of the energy spectrum of cosmic ray helium nuclei from 70 GeV to 80 TeV using 4.5 years of data recorded by the Dark Matter Particle Explorer (DAMPE) is reported in this work. A hardening of the spectrum is observed at an energy of about 1.3 TeV, similar to previous observations. In addition, a spectral softening at about 34 TeV is revealed for the first time with large statistics and well controlled systematic uncertainties, with an overall significance of 4.3σ. The DAMPE spectral measurements of both cosmic protons and helium nuclei suggest a particle charge dependent softening energy, although with current uncertainties a dependence on the number of nucleons cannot be ruled out.
Collapse
Affiliation(s)
- F Alemanno
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - Q An
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - P Azzarello
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - F C T Barbato
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - P Bernardini
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - X J Bi
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
| | - M S Cai
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - E Catanzani
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Perugia, I-06123 Perugia, Italy
| | - J Chang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - D Y Chen
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - J L Chen
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Z F Chen
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - M Y Cui
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - T S Cui
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Y X Cui
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - H T Dai
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - A D'Amone
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - A De Benedittis
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - I De Mitri
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - F de Palma
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - M Deliyergiyev
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - M Di Santo
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - T K Dong
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Z X Dong
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - G Donvito
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Bari, I-70125 Bari, Italy
| | - D Droz
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - J L Duan
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - K K Duan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - D D'Urso
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Perugia, I-06123 Perugia, Italy
| | - R R Fan
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - Y Z Fan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - K Fang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - F Fang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - C Q Feng
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - L Feng
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - P Fusco
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Bari, I-70125 Bari, Italy
- Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy
| | - M Gao
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - F Gargano
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Bari, I-70125 Bari, Italy
| | - K Gong
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - Y Z Gong
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - D Y Guo
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J H Guo
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - X L Guo
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - S X Han
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Y M Hu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - G S Huang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - X Y Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - Y Y Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - M Ionica
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Perugia, I-06123 Perugia, Italy
| | - W Jiang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - J Kong
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - A Kotenko
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - D Kyratzis
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - S J Lei
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - S Li
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - W L Li
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - X Li
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - X Q Li
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Y M Liang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - C M Liu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - H Liu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - J Liu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - S B Liu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - W Q Liu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y Liu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - F Loparco
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Bari, I-70125 Bari, Italy
- Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy
| | - C N Luo
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - M Ma
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - P X Ma
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - T Ma
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - X Y Ma
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - G Marsella
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - M N Mazziotta
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Bari, I-70125 Bari, Italy
| | - D Mo
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X Y Niu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X Pan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - A Parenti
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - W X Peng
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - X Y Peng
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - C Perrina
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - R Qiao
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J N Rao
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - A Ruina
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - M M Salinas
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - G Z Shang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - W H Shen
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Z Q Shen
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Z T Shen
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - L Silveri
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - J X Song
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - M Stolpovskiy
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - H Su
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - M Su
- Department of Physics and Laboratory for Space Research, the University of Hong Kong, Pok Fu Lam, Hong Kong SAR 999077, China
| | - Z Y Sun
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - A Surdo
- Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Lecce, I-73100 Lecce, Italy
| | - X J Teng
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - A Tykhonov
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - H Wang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - J Z Wang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - L G Wang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - S Wang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - X L Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y F Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y Z Wang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Z M Wang
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L'Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)-Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L'Aquila, Italy
| | - D M Wei
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - J J Wei
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Y F Wei
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - S C Wen
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - D Wu
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J Wu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - L B Wu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - S S Wu
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - X Wu
- Department of Nuclear and Particle Physics, University of Geneva, CH-1211 Geneva, Switzerland
| | - Z Q Xia
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - H T Xu
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Z H Xu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - Z L Xu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Z Z Xu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - G F Xue
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - H B Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - P Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y Q Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - H J Yao
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y H Yu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - G W Yuan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - Q Yuan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - C Yue
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - J J Zang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - F Zhang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - S X Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - W Z Zhang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Y Zhang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Y J Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y L Zhang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y P Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y Q Zhang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Z Zhang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Z Y Zhang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - C Zhao
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - H Y Zhao
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X F Zhao
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - C Y Zhou
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| | - Y Zhu
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian district, Beijing 100190, China
| |
Collapse
|
15
|
Boschini MJ, Della Torre S, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. The Discovery of a Low-energy Excess in Cosmic-Ray Iron: Evidence of the Past Supernova Activity in the Local Bubble. THE ASTROPHYSICAL JOURNAL 2021; 913:5. [PMID: 34646050 PMCID: PMC8506974 DOI: 10.3847/1538-4357/abf11c] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Since its launch, the Alpha Magnetic Spectrometer-02 (AMS-02) has delivered outstanding quality measurements of the spectra of cosmic-ray (CR) species ( p ¯ , e ±, and nuclei, 1H-8O, 10Ne, 12Mg, 14Si) which resulted in a number of breakthroughs. One of the latest long-awaited surprises is the spectrum of 26Fe just published by AMS-02. Because of the large fragmentation cross section and large ionization energy losses, most of CR iron at low energies is local and may harbor some features associated with relatively recent supernova (SN) activity in the solar neighborhood. Our analysis of the new AMS-02 results, together with Voyager 1 and ACE-CRIS data, reveals an unexpected bump in the iron spectrum and in the Fe/He, Fe/O, and Fe/Si ratios at 1-2 GV, while a similar feature in the spectra of He, O, and Si and in their ratios is absent, hinting at a local source of low-energy CRs. The found excess extends the recent discoveries of radioactive 60Fe deposits in terrestrial and lunar samples and in CRs. We provide an updated local interstellar spectrum (LIS) of iron in the energy range from 1 MeV nucleon-1 to ~10 TeV nucleon-1. Our calculations employ the GALPROP-HELMOD framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei Z ⩽ 28.
Collapse
Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| |
Collapse
|
16
|
Abstract
Continuum gamma-ray emission produced by interactions of cosmic rays with interstellar matter and radiation fields is a probe of non-thermal particle populations in galaxies. After decades of continuous improvements in experimental techniques and an ever-increasing sky and energy coverage, gamma-ray observations reveal in unprecedented detail the properties of galactic cosmic rays. A variety of scales and environments are now accessible to us, from the local interstellar medium near the Sun and the vicinity of cosmic-ray accelerators, out to the Milky Way at large and beyond, with a growing number of gamma-ray emitting star-forming galaxies. Gamma-ray observations have been pushing forward our understanding of the life cycle of cosmic rays in galaxies and, combined with advances in related domains, they have been challenging standard assumptions in the field and have spurred new developments in modelling approaches and data analysis methods. We provide a review of the status of the subject and discuss perspectives on future progress.
Collapse
|
17
|
Evoli C, Amato E, Blasi P, Aloisio R. Galactic factories of cosmic-ray electrons and positrons. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.103.083010] [Citation(s) in RCA: 26] [Impact Index Per Article: 8.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
18
|
Amenomori M, Bao YW, Bi XJ, Chen D, Chen TL, Chen WY, Chen X, Chen Y, Cui SW, Ding LK, Fang JH, Fang K, Feng CF, Feng Z, Feng ZY, Gao Q, Gou QB, Guo YQ, Guo YY, He HH, He ZT, Hibino K, Hotta N, Hu H, Hu HB, Huang J, Jia HY, Jiang L, Jin HB, Kasahara K, Katayose Y, Kato C, Kato S, Kawata K, Kihara W, Ko Y, Kozai M, Le GM, Li AF, Li HJ, Li WJ, Lin YH, Liu B, Liu C, Liu JS, Liu MY, Liu W, Lou YQ, Lu H, Meng XR, Munakata K, Nakada H, Nakamura Y, Nanjo H, Nishizawa M, Ohnishi M, Ohura T, Ozawa S, Qian XL, Qu XB, Saito T, Sakata M, Sako TK, Shao J, Shibata M, Shiomi A, Sugimoto H, Takano W, Takita M, Tan YH, Tateyama N, Torii S, Tsuchiya H, Udo S, Wang H, Wu HR, Xue L, Yamamoto Y, Yang Z, Yokoe Y, Yuan AF, Zhai LM, Zhang HM, Zhang JL, Zhang X, Zhang XY, Zhang Y, Zhang Y, Zhang Y, Zhao SP, Zhou XX. First Detection of sub-PeV Diffuse Gamma Rays from the Galactic Disk: Evidence for Ubiquitous Galactic Cosmic Rays beyond PeV Energies. PHYSICAL REVIEW LETTERS 2021; 126:141101. [PMID: 33891464 DOI: 10.1103/physrevlett.126.141101] [Citation(s) in RCA: 8] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/06/2020] [Revised: 01/05/2021] [Accepted: 01/21/2021] [Indexed: 06/12/2023]
Abstract
We report, for the first time, the long-awaited detection of diffuse gamma rays with energies between 100 TeV and 1 PeV in the Galactic disk. Particularly, all gamma rays above 398 TeV are observed apart from known TeV gamma-ray sources and compatible with expectations from the hadronic emission scenario in which gamma rays originate from the decay of π^{0}'s produced through the interaction of protons with the interstellar medium in the Galaxy. This is strong evidence that cosmic rays are accelerated beyond PeV energies in our Galaxy and spread over the Galactic disk.
Collapse
Affiliation(s)
- M Amenomori
- Department of Physics, Hirosaki University, Hirosaki 036-8561, Japan
| | - Y W Bao
- School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China
| | - X J Bi
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - D Chen
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
| | - T L Chen
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - W Y Chen
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Xu Chen
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Y Chen
- School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China
| | - S W Cui
- Department of Physics, Hebei Normal University, Shijiazhuang 050016, China
| | - L K Ding
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - J H Fang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - K Fang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - C F Feng
- Institute of Frontier and Interdisciplinary Science and Key Laboratory of Particle Physics and Particle Irradiation (MOE), Shandong University, Qingdao 266237, China
| | - Zhaoyang Feng
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Z Y Feng
- Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China
| | - Qi Gao
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - Q B Gou
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Y Q Guo
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Y Y Guo
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - H H He
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Z T He
- Department of Physics, Hebei Normal University, Shijiazhuang 050016, China
| | - K Hibino
- Faculty of Engineering, Kanagawa University, Yokohama 221-8686, Japan
| | - N Hotta
- Faculty of Education, Utsunomiya University, Utsunomiya 321-8505, Japan
| | - Haibing Hu
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - H B Hu
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - J Huang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - H Y Jia
- Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China
| | - L Jiang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - H B Jin
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
| | - K Kasahara
- Faculty of Systems Engineering, Shibaura Institute of Technology, Omiya 330-8570, Japan
| | - Y Katayose
- Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan
| | - C Kato
- Department of Physics, Shinshu University, Matsumoto 390-8621, Japan
| | - S Kato
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - K Kawata
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - W Kihara
- Department of Physics, Shinshu University, Matsumoto 390-8621, Japan
| | - Y Ko
- Department of Physics, Shinshu University, Matsumoto 390-8621, Japan
| | - M Kozai
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara 252-5210, Japan
| | - G M Le
- National Center for Space Weather, China Meteorological Administration, Beijing 100081, China
| | - A F Li
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
- Institute of Frontier and Interdisciplinary Science and Key Laboratory of Particle Physics and Particle Irradiation (MOE), Shandong University, Qingdao 266237, China
- School of Information Science and Engineering, Shandong Agriculture University, Taian 271018, China
| | - H J Li
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - W J Li
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
- Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China
| | - Y H Lin
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - B Liu
- Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China
| | - C Liu
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - J S Liu
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - M Y Liu
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - W Liu
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Y-Q Lou
- Department of Physics and Tsinghua Centre for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
- Tsinghua University-National Astronomical Observatories of China (NAOC) Joint Research Center for Astrophysics, Tsinghua University, Beijing 100084, China
- Department of Astronomy, Tsinghua University, Beijing 100084, China
| | - H Lu
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - X R Meng
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - K Munakata
- Department of Physics, Shinshu University, Matsumoto 390-8621, Japan
| | - H Nakada
- Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan
| | - Y Nakamura
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - H Nanjo
- Department of Physics, Hirosaki University, Hirosaki 036-8561, Japan
| | - M Nishizawa
- National Institute of Informatics, Tokyo 101-8430, Japan
| | - M Ohnishi
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - T Ohura
- Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan
| | - S Ozawa
- National Institute of Information and Communications Technology, Tokyo 184-8795, Japan
| | - X L Qian
- Department of Mechanical and Electrical Engineering, Shandong Management University, Jinan 250357, China
| | - X B Qu
- College of Science, China University of Petroleum, Qingdao, 266555, China
| | - T Saito
- Tokyo Metropolitan College of Industrial Technology, Tokyo 116-8523, Japan
| | - M Sakata
- Department of Physics, Konan University, Kobe 658-8501, Japan
| | - T K Sako
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - J Shao
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
- Institute of Frontier and Interdisciplinary Science and Key Laboratory of Particle Physics and Particle Irradiation (MOE), Shandong University, Qingdao 266237, China
| | - M Shibata
- Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan
| | - A Shiomi
- College of Industrial Technology, Nihon University, Narashino 275-8575, Japan
| | - H Sugimoto
- Shonan Institute of Technology, Fujisawa 251-8511, Japan
| | - W Takano
- Faculty of Engineering, Kanagawa University, Yokohama 221-8686, Japan
| | - M Takita
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - Y H Tan
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - N Tateyama
- Faculty of Engineering, Kanagawa University, Yokohama 221-8686, Japan
| | - S Torii
- Research Institute for Science and Engineering, Waseda University, Tokyo 169-8555, Japan
| | - H Tsuchiya
- Japan Atomic Energy Agency, Tokai-mura 319-1195, Japan
| | - S Udo
- Faculty of Engineering, Kanagawa University, Yokohama 221-8686, Japan
| | - H Wang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - H R Wu
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - L Xue
- Institute of Frontier and Interdisciplinary Science and Key Laboratory of Particle Physics and Particle Irradiation (MOE), Shandong University, Qingdao 266237, China
| | - Y Yamamoto
- Department of Physics, Konan University, Kobe 658-8501, Japan
| | - Z Yang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Y Yokoe
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan
| | - A F Yuan
- Physics Department of Science School, Tibet University, Lhasa 850000, China
| | - L M Zhai
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
| | - H M Zhang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - J L Zhang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - X Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China
| | - X Y Zhang
- Institute of Frontier and Interdisciplinary Science and Key Laboratory of Particle Physics and Particle Irradiation (MOE), Shandong University, Qingdao 266237, China
| | - Y Zhang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - Yi Zhang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210034, China
| | - Ying Zhang
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - S P Zhao
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
| | - X X Zhou
- Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China
| |
Collapse
|
19
|
Abstract
In the past few decades, many studies have analyzed the data of gamma-rays, X-rays, radio waves, electrons, positrons, anti-protons, and neutrinos to search for the signal of dark matter annihilation. In particular, analyzing radio data has been one of the most important and effective ways to constrain dark matter. In this article, we review the physics and the theoretical framework of using radio data to constrain annihilating dark matter. We also review some important radio constraints of annihilating dark matter and discuss the future perspectives of using radio detection to reveal the nature of dark matter.
Collapse
|
20
|
Motz H, Okada H, Asaoka Y, Kohri K. Cosmic-ray signatures of dark matter from a flavor dependent gauge symmetry model with neutrino mass mechanism. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.083019] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
21
|
Abstract
Indirect searches for dark matter are based on detecting an anomalous flux of photons, neutrinos or cosmic-rays produced in annihilations or decays of dark matter candidates gravitationally accumulated in heavy cosmological objects, like galaxies, the Sun or the Earth. Additionally, evidence for dark matter that can also be understood as indirect can be obtained from early universe probes, like fluctuations of the cosmic microwave background temperature, the primordial abundance of light elements or the Hydrogen 21-cm line. The techniques needed to detect these different signatures require very different types of detectors: Air shower arrays, gamma- and X-ray telescopes, neutrino telescopes, radio telescopes or particle detectors in balloons or satellites. While many of these detectors were not originally intended to search for dark matter, they have proven to be unique complementary tools for direct search efforts. In this review we summarize the current status of indirect searches for dark matter, mentioning also the challenges and limitations that these techniques encounter.
Collapse
|
22
|
Boschini MJ, Torre SD, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. Inference of the Local Interstellar Spectra of Cosmic-Ray Nuclei Z ⩽ 28 with the GalProp-HelMod Framework. THE ASTROPHYSICAL JOURNAL. SUPPLEMENT SERIES 2020; 250:27. [PMID: 34711999 PMCID: PMC8549769 DOI: 10.3847/1538-4365/aba901] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
Composition and spectra of Galactic cosmic rays (CRs) are vital for studies of high-energy processes in a variety of environments and on different scales, for interpretation of γ-ray and microwave observations, for disentangling possible signatures of new phenomena, and for understanding of our local Galactic neighborhood. Since its launch, AMS-02 has delivered outstanding-quality measurements of the spectra of p ¯ , e ±, and nuclei: 1H-8O, 10Ne, 12Mg, 14Si. These measurements resulted in a number of breakthroughs; however, spectra of heavier nuclei and especially low-abundance nuclei are not expected until later in the mission. Meanwhile, a comparison of published AMS-02 results with earlier data from HEAO-3-C2 indicates that HEAO-3-C2 data may be affected by undocumented systematic errors. Utilizing such data to compensate for the lack of AMS-02 measurements could result in significant errors. In this paper we show that a fraction of HEAO-3-C2 data match available AMS-02 measurements quite well and can be used together with Voyager 1 and ACE-CRIS data to make predictions for the local interstellar spectra (LIS) of nuclei that are not yet released by AMS-02. We are also updating our already-published LIS to provide a complete set from 1H-28Ni in the energy range from 1 MeV nucleon-1 to ~100-500 TeV nucleon-1, thus covering 8-9 orders of magnitude in energy. Our calculations employ the GalProp-HelMod framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei 1H-8O.
Collapse
Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, 106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| |
Collapse
|
23
|
Cosmic-Ray Database Update: Ultra-High Energy, Ultra-Heavy, and Antinuclei Cosmic-Ray Data (CRDB v4.0). UNIVERSE 2020. [DOI: 10.3390/universe6080102] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
We present an update on CRDB, the cosmic-ray database for charged species. CRDB is based on MySQL, queried and sorted by jquery and table-sorter libraries, and displayed via PHP web pages through the AJAX protocol. We review the modifications made on the structure and outputs of the database since the first release (Maurin et al., 2014). For this update, the most important feature is the inclusion of ultra-heavy nuclei (Z>30), ultra-high energy nuclei (from 1015 to 1020 eV), and limits on antinuclei fluxes (Z≤−1 for A>1); more than 100 experiments, 350 publications, and 40,000 data points are now available in CRDB. We also revisited and simplified how users can retrieve data and submit new ones. For questions and requests, please contact crdb@lpsc.in2p3.fr.
Collapse
|
24
|
Evoli C, Morlino G, Blasi P, Aloisio R. AMS-02 beryllium data and its implication for cosmic ray transport. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.023013] [Citation(s) in RCA: 47] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
25
|
Lu J, Wang SH, Li Y, Wang WF, Sun C, Li PX, Zheng FK, Guo GC. Heat-resistant Pb(ii)-based X-ray scintillating metal–organic frameworks for sensitive dosage detection via an aggregation-induced luminescent chromophore. Dalton Trans 2020; 49:7309-7314. [DOI: 10.1039/d0dt00974a] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
Unusual X-aggregation induced luminescent chromophores in heat-resistant Pb(ii)-based metal–organic frameworks facilitate excellent scintillation for X-ray dosage detection.
Collapse
Affiliation(s)
- Jian Lu
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Shuai-Hua Wang
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Yan Li
- Key Laboratory of Optoelectronic Materials Chemistry and Physics
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Wen-Fei Wang
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Cai Sun
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Pei-Xin Li
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Fa-Kun Zheng
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| | - Guo-Cong Guo
- State Key Laboratory of Structural Chemistry
- Fujian Institute of Research on the Structure of Matter
- Chinese Academy of Sciences
- Fuzhou
- P. R. China
| |
Collapse
|
26
|
Schael S, Atanasyan A, Berdugo J, Bretz T, Czupalla M, Dachwald B, von Doetinchem P, Duranti M, Gast H, Karpinski W, Kirn T, Lübelsmeyer K, Maña C, Marrocchesi PS, Mertsch P, Moskalenko IV, Schervan T, Schluse M, Schröder KU, Schultz von Dratzig A, Senatore C, Spies L, Wakely SP, Wlochal M, Uglietti D, Zimmermann J. AMS-100: The Next Generation Magnetic Spectrometer in Space - An International Science Platform for Physics and Astrophysics at Lagrange Point 2. NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH. SECTION A, ACCELERATORS, SPECTROMETERS, DETECTORS AND ASSOCIATED EQUIPMENT 2019; 944:162561. [PMID: 34646055 PMCID: PMC8506902 DOI: 10.1016/j.nima.2019.162561] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
The next generation magnetic spectrometer in space, AMS-100, is designed to have a geometrical acceptance of 100 m2 sr and to be operated for at least ten years at the Sun-Earth Lagrange Point 2. Compared to existing experiments, it will improve the sensitivity for the observation of new phenomena in cosmic rays, and in particular in cosmic antimatter, by at least a factor of 1000. The magnet design is based on high temperature superconductor tapes, which allow the construction of a thin solenoid with a homogeneous magnetic field of 1 Tesla inside. The inner volume is instrumented with a silicon tracker reaching a maximum detectable rigidity of 100 TV and a calorimeter system that is 70 radiation lengths deep, equivalent to four nuclear interaction lengths, which extends the energy reach for cosmic-ray nuclei up to the PeV scale, i.e. beyond the cosmic-ray knee. Covering most of the sky continuously, AMS-100 will detect high-energy gamma rays in the calorimeter system and by pair conversion in the thin solenoid, reconstructed with excellent angular resolution in the silicon tracker.
Collapse
Affiliation(s)
- S. Schael
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - A. Atanasyan
- Institut für Mensch-Maschine-Interaktion, RWTH Aachen University, Ahornstr. 55, 52074 Aachen, Germany
| | - J. Berdugo
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Av. Complutense 40, 28040 Madrid, Spain
| | - T. Bretz
- III. Physikalisches Institut A, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - M. Czupalla
- Fachbereich Luft- und Raumfahrttechnik, Fachhochschule Aachen, Hohenstaufenallee 6, 52064 Aachen, Germany
| | - B. Dachwald
- Fachbereich Luft- und Raumfahrttechnik, Fachhochschule Aachen, Hohenstaufenallee 6, 52064 Aachen, Germany
| | - P. von Doetinchem
- Physics and Astronomy Department, University of Hawaii, Honolulu, HI, 96822, U.S.A
| | - M. Duranti
- INFN Sezione di Perugia, 06100 Perugia, Italy
| | - H. Gast
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - W. Karpinski
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - T. Kirn
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - K. Lübelsmeyer
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - C. Maña
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Av. Complutense 40, 28040 Madrid, Spain
| | - P. S. Marrocchesi
- Department of Physical Sciences, Earth and Environment, University of Siena and INFN Sezione di Pisa, 53100 Siena, Italy
| | - P. Mertsch
- Institut für Theoretische Teilchenphysik und Kosmologie, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - I. V. Moskalenko
- W.W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA, 94305, U.S.A
| | - T. Schervan
- Institut für Strukturmechanik und Leichtbau, RWTH Aachen University, Wüllnerstr. 7, 52062 Aachen, Germany
| | - M. Schluse
- Institut für Mensch-Maschine-Interaktion, RWTH Aachen University, Ahornstr. 55, 52074 Aachen, Germany
| | - K.-U. Schröder
- Institut für Strukturmechanik und Leichtbau, RWTH Aachen University, Wüllnerstr. 7, 52062 Aachen, Germany
| | - A. Schultz von Dratzig
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - C. Senatore
- Department of Quantum Matter Physics, Université de Genève, 24 Quai Ernest-Ansermet, 1211 Geneva, Switzerland
| | - L. Spies
- Fachbereich Luft- und Raumfahrttechnik, Fachhochschule Aachen, Hohenstaufenallee 6, 52064 Aachen, Germany
| | - S. P. Wakely
- Enrico Fermi Institute, University of Chicago, Chicago, IL, 60637, U.S.A
| | - M. Wlochal
- I. Physikalisches Institut, RWTH Aachen University, Sommerfeldstr. 14, 52074 Aachen, Germany
| | - D. Uglietti
- Ecole Polytechnique Fédérale de Lausanne (EPFL), Swiss Plasma Center (SPC), 5232 Villigen PSI, Switzerland
| | - J. Zimmermann
- Institut für Strukturmechanik und Leichtbau, RWTH Aachen University, Wüllnerstr. 7, 52062 Aachen, Germany
| |
Collapse
|
27
|
An Q, Asfandiyarov R, Azzarello P, Bernardini P, Bi XJ, Cai MS, Chang J, Chen DY, Chen HF, Chen JL, Chen W, Cui MY, Cui TS, Dai HT, D’Amone A, De Benedittis A, De Mitri I, Di Santo M, Ding M, Dong TK, Dong YF, Dong ZX, Donvito G, Droz D, Duan JL, Duan KK, D’Urso D, Fan RR, Fan YZ, Fang F, Feng CQ, Feng L, Fusco P, Gallo V, Gan FJ, Gao M, Gargano F, Gong K, Gong YZ, Guo DY, Guo JH, Guo XL, Han SX, Hu YM, Huang GS, Huang XY, Huang YY, Ionica M, Jiang W, Jin X, Kong J, Lei SJ, Li S, Li WL, Li X, Li XQ, Li Y, Liang YF, Liang YM, Liao NH, Liu CM, Liu H, Liu J, Liu SB, Liu WQ, Liu Y, Loparco F, Luo CN, Ma M, Ma PX, Ma SY, Ma T, Ma XY, Marsella G, Mazziotta MN, Mo D, Niu XY, Pan X, Peng WX, Peng XY, Qiao R, Rao JN, Salinas MM, Shang GZ, Shen WH, Shen ZQ, Shen ZT, Song JX, Su H, Su M, Sun ZY, Surdo A, Teng XJ, Tykhonov A, Vitillo S, Wang C, Wang H, Wang HY, Wang JZ, Wang LG, Wang Q, Wang S, Wang XH, Wang XL, Wang YF, Wang YP, Wang YZ, Wang ZM, Wei DM, Wei JJ, Wei YF, Wen SC, Wu D, Wu J, Wu LB, Wu SS, Wu X, Xi K, Xia ZQ, Xu HT, Xu ZH, Xu ZL, Xu ZZ, Xue GF, Yang HB, Yang P, Yang YQ, Yang ZL, Yao HJ, Yu YH, Yuan Q, Yue C, Zang JJ, Zhang F, Zhang JY, Zhang JZ, Zhang PF, Zhang SX, Zhang WZ, Zhang Y, Zhang YJ, Zhang YL, Zhang YP, Zhang YQ, Zhang Z, Zhang ZY, Zhao H, Zhao HY, Zhao XF, Zhou CY, Zhou Y, Zhu X, Zhu Y, Zimmer S. Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite. SCIENCE ADVANCES 2019; 5:eaax3793. [PMID: 31799401 PMCID: PMC6868675 DOI: 10.1126/sciadv.aax3793] [Citation(s) in RCA: 21] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/18/2019] [Accepted: 09/03/2019] [Indexed: 05/23/2023]
Abstract
The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2 1/2 years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.
Collapse
Affiliation(s)
| | - Q. An
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - R. Asfandiyarov
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - P. Azzarello
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - P. Bernardini
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Lecce, I-73100 Lecce, Italy
| | - X. J. Bi
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
| | - M. S. Cai
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - J. Chang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - D. Y. Chen
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - H. F. Chen
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - J. L. Chen
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - W. Chen
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - M. Y. Cui
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - T. S. Cui
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - H. T. Dai
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - A. D’Amone
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Lecce, I-73100 Lecce, Italy
| | - A. De Benedittis
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Lecce, I-73100 Lecce, Italy
| | - I. De Mitri
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L’Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Laboratori Nazionali del Gran Sasso, Assergi, I-67100 L’Aquila, Italy
| | - M. Di Santo
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Lecce, I-73100 Lecce, Italy
| | - M. Ding
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - T. K. Dong
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Y. F. Dong
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - Z. X. Dong
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - G. Donvito
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Bari, I-70125, Bari, Italy
| | - D. Droz
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - J. L. Duan
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - K. K. Duan
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - D. D’Urso
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Perugia, I-06123 Perugia, Italy
| | - R. R. Fan
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - Y. Z. Fan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - F. Fang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - C. Q. Feng
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - L. Feng
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - P. Fusco
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Bari, I-70125, Bari, Italy
- Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari, I-70126 Bari, Italy
| | - V. Gallo
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - F. J. Gan
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - M. Gao
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - F. Gargano
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Bari, I-70125, Bari, Italy
| | - K. Gong
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - Y. Z. Gong
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - D. Y. Guo
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J. H. Guo
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - X. L. Guo
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - S. X. Han
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Y. M. Hu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - G. S. Huang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - X. Y. Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Y. Y. Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - M. Ionica
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Perugia, I-06123 Perugia, Italy
| | - W. Jiang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - X. Jin
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - J. Kong
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - S. J. Lei
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - S. Li
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - W. L. Li
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - X. Li
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - X. Q. Li
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Y. Li
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y. F. Liang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Y. M. Liang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - N. H. Liao
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - C. M. Liu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - H. Liu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - J. Liu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - S. B. Liu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - W. Q. Liu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y. Liu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - F. Loparco
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Bari, I-70125, Bari, Italy
- Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari, I-70126 Bari, Italy
| | - C. N. Luo
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - M. Ma
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - P. X. Ma
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - S. Y. Ma
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - T. Ma
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - X. Y. Ma
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - G. Marsella
- Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100 Lecce, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Lecce, I-73100 Lecce, Italy
| | - M. N. Mazziotta
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Bari, I-70125, Bari, Italy
| | - D. Mo
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X. Y. Niu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X. Pan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - W. X. Peng
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - X. Y. Peng
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - R. Qiao
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J. N. Rao
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - M. M. Salinas
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - G. Z. Shang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - W. H. Shen
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Z. Q. Shen
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Z. T. Shen
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - J. X. Song
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - H. Su
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - M. Su
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- Department of Physics and Laboratory for Space Research, The University of Hong Kong, Pok Fu Lam, Hong Kong, China
| | - Z. Y. Sun
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - A. Surdo
- Istituto Nazionale di Fisica Nucleare (INFN)–Sezione di Lecce, I-73100 Lecce, Italy
| | - X. J. Teng
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - A. Tykhonov
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - S. Vitillo
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - C. Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - H. Wang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - H. Y. Wang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J. Z. Wang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - L. G. Wang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Q. Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - S. Wang
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - X. H. Wang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X. L. Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y. F. Wang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y. P. Wang
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Y. Z. Wang
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Z. M. Wang
- Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L’Aquila, Italy
- Istituto Nazionale di Fisica Nucleare (INFN)–Laboratori Nazionali del Gran Sasso, Assergi, I-67100 L’Aquila, Italy
| | - D. M. Wei
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - J. J. Wei
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Y. F. Wei
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - S. C. Wen
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - D. Wu
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J. Wu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - L. B. Wu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - S. S. Wu
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - X. Wu
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| | - K. Xi
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Z. Q. Xia
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - H. T. Xu
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Z. H. Xu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - Z. L. Xu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Z. Z. Xu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - G. F. Xue
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - H. B. Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - P. Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y. Q. Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Z. L. Yang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - H. J. Yao
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y. H. Yu
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Q. Yuan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
| | - C. Yue
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - J. J. Zang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - F. Zhang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J. Y. Zhang
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - J. Z. Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - P. F. Zhang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - S. X. Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - W. Z. Zhang
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Y. Zhang
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Y. J. Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y. L. Zhang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y. P. Zhang
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - Y. Q. Zhang
- University of Chinese Academy of Sciences, Yuquan Road 19A, Beijing 100049, China
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Z. Zhang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
| | - Z. Y. Zhang
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - H. Zhao
- Institute of High Energy Physics, Chinese Academy of Sciences, Yuquan Road 19B, Beijing 100049, China
| | - H. Y. Zhao
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X. F. Zhao
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - C. Y. Zhou
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - Y. Zhou
- Institute of Modern Physics, Chinese Academy of Sciences, Nanchang Road 509, Lanzhou 730000, China
| | - X. Zhu
- State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
- Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
| | - Y. Zhu
- National Space Science Center, Chinese Academy of Sciences, Nanertiao 1, Zhongguancun, Haidian District, Beijing 100190, China
| | - S. Zimmer
- Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
| |
Collapse
|
28
|
Diesing R, Caprioli D. Spectrum of Electrons Accelerated in Supernova Remnants. PHYSICAL REVIEW LETTERS 2019; 123:071101. [PMID: 31491115 DOI: 10.1103/physrevlett.123.071101] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/17/2019] [Indexed: 06/10/2023]
Abstract
Using a semianalytic model of nonlinear diffusive shock acceleration, we model the total spectrum of cosmic ray (CR) electrons accelerated by supernova remnants (SNRs). Because electrons experience synchrotron losses in the amplified magnetic fields characteristic of SNRs, they exhibit substantially steeper spectra than protons. In particular, we find that the difference between the electron and proton spectral index (power law slope) ranges from 0.1 to 0.4. Our findings must be reckoned with theories of Galactic CR transport, which often assume that electrons and protons are injected with the same slope, and may especially have implications for the observed "positron excess".
Collapse
Affiliation(s)
- Rebecca Diesing
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
| | - Damiano Caprioli
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
| |
Collapse
|
29
|
|
30
|
Recchia S, Gabici S, Aharonian F, Vink J. Local fading accelerator and the origin of TeV cosmic ray electrons. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.103022] [Citation(s) in RCA: 17] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
31
|
On the Gamma-Ray Nebula of Vela Pulsar. I. Very Slow Diffusion of Energetic Electrons within the TeV Nebula. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab1908] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
|
32
|
Abstract
The High Energy cosmic-Radiation Detection (HERD) facility will be one of the space astronomy payloads on board the future Chinese space station. The ambitious aim of HERD is the direct detection of cosmic rays towards the “knee” region (~ 1 PeV), with a detector able to measure electrons, photons and nuclei with an excellent energy resolution (1% for electrons and photons at 200 GeV and 20% for nuclei at 100 GeV - PeV), an acceptance 10 times the one of present generation missions (~ 1 m2 sr), and long life-time (> 10 years). The primary objectives of HERD are the indirect search for dark matter particles and the precise measurement of energy distribution and composition of cosmic rays from 30 GeV up to a few PeV, determining the origin of the “knee” structure of the spectrum. Furthermore, HERD will monitor the high energy gamma-ray sky from 500 MeV, observing gamma-ray bursts, active galactic nuclei, galactic microquasars, etc. HERD will be composed of a homogeneous calorimeter, surrounded by a particle tracker and a plastic scintillator detector. Two possible trackers are under study: a 5-side tracker made of silicon strip detectors and a 4-side scintillating fiber tracker with a silicon strip top tracker. The total volume of HERD will be (2.3 × 2.3 × 2.6) m3 with a weight of about 4 t. The HERD design, perspectives, expected performances in terms of energy sensitivity and acceptance will be presented in this contribution.
Collapse
|
33
|
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 MJ, Bourquin M, Bueno EF, Burger J, Burger WJ, Cai XD, Capell M, Caroff S, Casaus J, Castellini G, Cervelli F, Chang YH, Chen GM, Chen HS, Chen Y, Cheng L, Chou HY, Choutko V, Chung CH, Clark C, Coignet G, Consolandi C, Contin A, Corti C, Crispoltoni M, Cui Z, Dadzie K, Dai YM, Datta A, Delgado C, Della Torre S, Demirköz MB, 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 RJ, Gargiulo C, Gast H, Gebauer I, Gervasi M, Giovacchini F, Gómez-Coral DM, Gong J, Goy C, Grabski V, Grandi D, Graziani M, Guo KH, Haino S, Han KC, He ZH, Heil M, Hsieh TH, Huang H, Huang ZC, Incagli M, Jia Y, Jinchi H, Kanishev K, Khiali B, Kirn T, Konak C, Kounina O, Kounine A, Koutsenko V, Kulemzin A, La Vacca G, Laudi E, Laurenti G, Lazzizzera I, Lebedev A, Lee HT, Lee SC, Leluc C, Li JQ, Li Q, Li TX, Li ZH, Light C, Lin CH, Lippert T, Liu FZ, Liu H, Liu Z, Lu SQ, Lu YS, Luebelsmeyer K, Luo F, Luo JZ, Luo X, Lyu SS, Machate F, Mañá C, Marín J, Martin T, Martínez G, Masi N, Maurin D, Menchaca-Rocha A, Meng Q, Mo DC, Molero M, Mott P, Mussolin L, Nelson T, Ni JQ, Nikonov N, Nozzoli F, Oliva A, Orcinha M, Palermo M, Palmonari F, Paniccia M, Pashnin A, Pauluzzi M, Pensotti S, Perrina C, Phan HD, Picot-Clemente N, Plyaskin V, Pohl M, Poireau V, Popkow A, Quadrani L, Qi XM, Qin X, Qu ZY, Rancoita PG, Rapin D, Conde AR, Rosier-Lees S, Rozhkov A, Rozza D, Sagdeev R, Solano C, Schael S, Schmidt SM, von Dratzig AS, Schwering G, Seo ES, Shan BS, Shi JY, Siedenburg T, Song JW, Sun ZT, Tacconi M, Tang XW, Tang ZC, Tian J, Ting SCC, Ting SM, Tomassetti N, Torsti J, Urban T, Vagelli V, Valente E, Valtonen E, Acosta MV, Vecchi M, Velasco M, Vialle JP, Vizán J, Wang LQ, Wang NH, Wang QL, Wang X, Wang XQ, Wang ZX, Wei J, Weng ZL, Wu H, Xiong RQ, Xu W, Yan Q, Yang Y, Yi H, Yu YJ, Yu ZQ, Zannoni M, Zeissler S, Zhang C, Zhang F, Zhang JH, Zhang Z, Zhao F, Zheng ZM, Zhuang HL, Zhukov V, Zichichi A, Zimmermann N, Zuccon P. Towards Understanding the Origin of Cosmic-Ray Electrons. PHYSICAL REVIEW LETTERS 2019; 122:101101. [PMID: 30932626 DOI: 10.1103/physrevlett.122.101101] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/07/2019] [Indexed: 06/09/2023]
Abstract
Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1×10^{6} 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.
Collapse
Affiliation(s)
- M Aguilar
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Ali Cavasonza
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - B Alpat
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - G Ambrosi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - L Arruda
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - N Attig
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - P Azzarello
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Bachlechner
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Barao
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - A Barrau
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - L Barrin
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | | | - L Basara
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - S Başeğmez-du Pree
- KVI-Center for Advanced Radiation Technology, University of Groningen, NL-9700 AB Groningen, Netherlands
| | - R Battiston
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - U Becker
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Behlmann
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - B Beischer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J Berdugo
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - B Bertucci
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - V Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - W de Boer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K Bollweg
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - B Borgia
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - M J Boschini
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M Bourquin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - E F Bueno
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - J Burger
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - X D Cai
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Capell
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Caroff
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - J Casaus
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | | | - F Cervelli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - Y H Chang
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan, 32054, Taiwan
| | - G M Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - H S Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Y Chen
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - L Cheng
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - H Y Chou
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan, 32054, Taiwan
| | - V Choutko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - C H Chung
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Clark
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - G Coignet
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - C Consolandi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - A Contin
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - C Corti
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - M Crispoltoni
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Z Cui
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - K Dadzie
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y M Dai
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - A Datta
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C Delgado
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - S Della Torre
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M B Demirköz
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - L Derome
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - S Di Falco
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - V Di Felice
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - F Dimiccoli
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - C Díaz
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P von Doetinchem
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Dong
- Southeast University (SEU), Nanjing, 210096, China
| | - F Donnini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - M Duranti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - A Egorov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Eline
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T Eronen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - J Feng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - E Fiandrini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - P Fisher
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Formato
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Y Galaktionov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - R J García-López
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - C Gargiulo
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - H Gast
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - I Gebauer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - M Gervasi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - F Giovacchini
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - D M Gómez-Coral
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - J Gong
- Southeast University (SEU), Nanjing, 210096, China
| | - C Goy
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - V Grabski
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - D Grandi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - M Graziani
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K H Guo
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - S Haino
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - K C Han
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan
| | - Z H He
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Heil
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T H Hsieh
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Huang
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - Z C Huang
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Incagli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - Yi Jia
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Jinchi
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan
| | | | - B Khiali
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Th Kirn
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Konak
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - O Kounina
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kounine
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Koutsenko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kulemzin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G La Vacca
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - E Laudi
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - G Laurenti
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - I Lazzizzera
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - A Lebedev
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H T Lee
- Academia Sinica Grid Center (ASGC), Nankang, Taipei, 11529, Taiwan
| | - S C Lee
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - C Leluc
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - J Q Li
- Southeast University (SEU), Nanjing, 210096, China
| | - Q Li
- Southeast University (SEU), Nanjing, 210096, China
| | - T X Li
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - Z H Li
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - C Light
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C H Lin
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - T Lippert
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - F Z Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Hu Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan, 32054, Taiwan
| | - Z Liu
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - S Q Lu
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - Y S Lu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - K Luebelsmeyer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Luo
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - J Z Luo
- Southeast University (SEU), Nanjing, 210096, China
| | - Xi Luo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S S Lyu
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - F Machate
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Mañá
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J Marín
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - T Martin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - G Martínez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - N Masi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - D Maurin
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - A Menchaca-Rocha
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - Q Meng
- Southeast University (SEU), Nanjing, 210096, China
| | - D C Mo
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Molero
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P Mott
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - L Mussolin
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - T Nelson
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J Q Ni
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - N Nikonov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Nozzoli
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - A Oliva
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - M Orcinha
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - M Palermo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Palmonari
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - M Paniccia
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Pashnin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pauluzzi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - S Pensotti
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - C Perrina
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - H D Phan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - V Plyaskin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pohl
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - V Poireau
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - A Popkow
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - L Quadrani
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - X M Qi
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - X Qin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z Y Qu
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - P G Rancoita
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - D Rapin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Reina Conde
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - S Rosier-Lees
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - A Rozhkov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - D Rozza
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - R Sagdeev
- East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA
| | - C Solano
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Schael
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - S M Schmidt
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - A Schulz von Dratzig
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - G Schwering
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - E S Seo
- IPST, University of Maryland, College Park, Maryland 20742, USA
| | - B S Shan
- Beihang University (BUAA), Beijing 100191, China
| | - J Y Shi
- Southeast University (SEU), Nanjing, 210096, China
| | - T Siedenburg
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J W Song
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - Z T Sun
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - M Tacconi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - X W Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - Z C Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J Tian
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Samuel C C Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - S M Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - N Tomassetti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - J Torsti
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - T Urban
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - V Vagelli
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - E Valente
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - E Valtonen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - M Vázquez Acosta
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - M Vecchi
- KVI-Center for Advanced Radiation Technology, University of Groningen, NL-9700 AB Groningen, Netherlands
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - M Velasco
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J P Vialle
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - J Vizán
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Q Wang
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - N H Wang
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - Q L Wang
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - X Wang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - X Q Wang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Z X Wang
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - J Wei
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - Z L Weng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Wu
- Southeast University (SEU), Nanjing, 210096, China
| | - R Q Xiong
- Southeast University (SEU), Nanjing, 210096, China
| | - W Xu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Q Yan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y Yang
- National Cheng Kung University, Tainan, 70101, Taiwan
| | - H Yi
- Southeast University (SEU), Nanjing, 210096, China
| | - Y J Yu
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - Z Q Yu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - M Zannoni
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - S Zeissler
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - C Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - F Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J H Zhang
- Southeast University (SEU), Nanjing, 210096, China
| | - Z Zhang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Zhao
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Z M Zheng
- Beihang University (BUAA), Beijing 100191, China
| | - H L Zhuang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - V Zhukov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - A Zichichi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - N Zimmermann
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - P Zuccon
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| |
Collapse
|
34
|
Abstract
There is a commonly expressed opinion in the literature, that cosmic-ray (CR) e+ come from a primary source, which could be dark matter or pulsars. In these proceedings we review some evidence to the contrary: namely, that e+ come from secondary production due to CR nuclei scattering on interstellar matter. We show that recent measurements of the total e± flux at E ≲ 3 TeV are in good agreement with the predicted flux of secondary e±, that would be obtained if radiative energy losses during CR propagation do not play an important role. If the agreement between data and secondary prediction is not accidental, then the requirement of negligible radiative energy losses implies a very short propagation time for high energy CRs: tesc ≲. 105 yr at rigidities R ≳ 3 TV. Such short propagation history may imply that a recent, near-by source dominates the CRs at these energies. We review independent evidence for a transition in CR propagation, based on the spectral hardening of primary and secondary nuclei around R ~ 100 GV. The transition rigidity of the nuclei matches the rigidity at which the e+ flux saturates its secondary upper bound.
Collapse
|
35
|
Abstract
DAMPE (DArk Matter Particle Explorer) is a satellite-born experiment, resulting from the collaboration of Chinese, Italian, and Swiss institutions. Since December 2015, DAMPE flights at the altitude of 500 km and collects data smoothly. The detector is made of four sub-detectors: top layers of plastic scintillators, a silicon-tungsten tracker, a BGO calorimeter (32 radiation lengths), and a bottom boron-doped scintillator to detect delayed neutrons. The main goal of the experiment is the search for indirect signals of Dark Matter in the electron and photon spectra with energies up to 10 TeV. Furthermore DAMPE studies cosmic charged and gamma radiation. The calorimeter depth and the large acceptance allow to measure cosmic ray fluxes in the range from 20 GeV up to hundreds of TeV. An overview of the latest results about light component (p+He) of charged cosmic rays, gamma astronomy and electron and positron spectrum will be presented.
Collapse
|
36
|
Asaoka Y, Adriani O, Akaike Y, Asano K, Bagliesi MG, Berti E, Bigongiari G, Binns WR, Bonechi S, Bongi M, Bruno A, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hasebe N, Hibinov K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kohri K, Krawczynski HS, Krizmanic JF, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, De Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Pal'shin V, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Sugita S, Suh JE, Sulaj A, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K. The CALorimetric Electron Telescope (CALET) on the International Space Station: Results from the First Two Years of Operation. EPJ WEB OF CONFERENCES 2019. [DOI: 10.1051/epjconf/201920813001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The CALorimetric Electron Telescope (CALET) space experiment, which has been developed by Japan in collaboration with Italy and the United States, is a high-energy astroparticle physics mission on the International Space Station (ISS). The primary goals of the CALET mission include investigation of possible nearby sources of high-energy electrons, detailed study of galactic cosmic-ray acceleration and propagation, and search for dark matter signatures. With a long-term observation onboard the ISS, the CALET experiment measures the flux of cosmic-ray electrons (including positrons) up to 20 TeV, gamma-rays to 10 TeV, and nuclei up to 1,000 TeV based on its charge separation capability from Z = 1 to 40. Since the start of science operation in mid-October, 2015, a continuous observation has been maintained without any major interruptions. The number of triggered events over 10 GeV is nearly 20 million per month. By using the data obtained during the first two-years, here we present a summary of the CALET observations: 1) Electron+positron energy spectrum, 2) Nuclei analysis, 3) Gamma-ray observation with a characterization of the on-orbit performance. The search results for the electromagnetic counterparts of LIGO/Virgo gravitational wave events are also discussed.
Collapse
|
37
|
López-Coto R, Parsons RD, Hinton JA, Giacinti G. Undiscovered Pulsar in the Local Bubble as an Explanation of the Local High Energy Cosmic Ray All-Electron Spectrum. PHYSICAL REVIEW LETTERS 2018; 121:251106. [PMID: 30608860 DOI: 10.1103/physrevlett.121.251106] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/13/2018] [Revised: 10/12/2018] [Indexed: 06/09/2023]
Abstract
Cosmic ray electrons and positrons are tracers of particle propagation in the interstellar medium (ISM). A recent measurement performed using the High Energy Stereoscopic System extends the all-electron (electron+positron) spectrum up to 20 TeV, probing very local sources and transport due to the ∼10 kyr cooling time of these particles. An additional key local measurement was the recent estimation of the ISM diffusion coefficient around Geminga performed using the High-Altitude Water Cherenkov Observatory. The inferred diffusion coefficient is much lower than typically assumed values. It has been argued that if this diffusion coefficient is representative of the local ISM, pulsars would not be able to account for the all-electron spectrum measured at Earth. Here we show that a low diffusion coefficient in the local ISM is compatible with a pulsar wind nebula origin of the highest energy electrons, if a so-far-undiscovered pulsar with spin-down power ∼10^{33-34} erg/s exists within 30-80 pc of Earth. The existence of such a pulsar is broadly consistent with the known population and may be detected in near future survey observations.
Collapse
Affiliation(s)
- R López-Coto
- INFN and Università di Padova, I-35131 Padova, Italy
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany
| | - R D Parsons
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany
| | - J A Hinton
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany
| | - G Giacinti
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany
| |
Collapse
|
38
|
Jin HB, Yue B, Zhang X, Chen X. Dark matter explanation of the cosmic ray
e+e−
spectrum excess and peak feature observed by the DAMPE experiment. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.123008] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
39
|
Archer A, Benbow W, Bird R, Brose R, Buchovecky M, Buckley J, Bugaev V, Connolly M, Cui W, Daniel M, Feng Q, Finley J, Fortson L, Furniss A, Gillanders G, Hütten M, Hanna D, Hervet O, Holder J, Hughes G, Humensky T, Johnson C, Kaaret P, Kar P, Kelley-Hoskins N, Kertzman M, Kieda D, Krause M, Krennrich F, Kumar S, Lang M, Lin T, Maier G, McArthur S, Moriarty P, Mukherjee R, O’Brien S, Ong R, Otte A, Petrashyk A, Pohl M, Pueschel E, Quinn J, Ragan K, Reynolds P, Richards G, Roache E, Rulten C, Sadeh I, Santander M, Sembroski G, Staszak D, Sushch I, Wakely S, Wells R, Wilcox P, Wilhelm A, Williams D, Williamson T, Zitzer B. Measurement of cosmic-ray electrons at TeV energies by VERITAS. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.062004] [Citation(s) in RCA: 20] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
40
|
|
41
|
Mazziotta M, Costanza F, Cuoco A, Gargano F, Loparco F, Zimmer S. Search for features in the cosmic-ray electron and positron spectrum measured by the Fermi Large Area Telescope. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.022006] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
42
|
Adriani O, Akaike Y, Asano K, Asaoka Y, Bagliesi MG, Berti E, Bigongiari G, Binns WR, Bonechi S, Bongi M, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hareyama M, Hasebe N, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kohri K, Krawczynski HS, Krizmanic JF, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, de Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Suh JE, Sulaj A, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K. Extended Measurement of the Cosmic-Ray Electron and Positron Spectrum from 11 GeV to 4.8 TeV with the Calorimetric Electron Telescope on the International Space Station. PHYSICAL REVIEW LETTERS 2018; 120:261102. [PMID: 30004739 DOI: 10.1103/physrevlett.120.261102] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/16/2018] [Revised: 05/21/2018] [Indexed: 06/08/2023]
Abstract
Extended results on the cosmic-ray electron + positron spectrum from 11 GeV to 4.8 TeV are presented based on observations with the Calorimetric Electron Telescope (CALET) on the International Space Station utilizing the data up to November 2017. The analysis uses the full detector acceptance at high energies, approximately doubling the statistics compared to the previous result. CALET is an all-calorimetric instrument with a total thickness of 30 X_{0} at normal incidence and fine imaging capability, designed to achieve large proton rejection and excellent energy resolution well into the TeV energy region. The observed energy spectrum in the region below 1 TeV shows good agreement with Alpha Magnetic Spectrometer (AMS-02) data. In the energy region below ∼300 GeV, CALET's spectral index is found to be consistent with the AMS-02, Fermi Large Area Telescope (Fermi-LAT), and Dark Matter Particle Explorer (DAMPE), while from 300 to 600 GeV the spectrum is significantly softer than the spectra from the latter two experiments. The absolute flux of CALET is consistent with other experiments at around a few tens of GeV. However, it is lower than those of DAMPE and Fermi-LAT with the difference increasing up to several hundred GeV. The observed energy spectrum above ∼1 TeV suggests a flux suppression consistent within the errors with the results of DAMPE, while CALET does not observe any significant evidence for a narrow spectral feature in the energy region around 1.4 TeV. Our measured all-electron flux, including statistical errors and a detailed breakdown of the systematic errors, is tabulated in the Supplemental Material in order to allow more refined spectral analyses based on our data.
Collapse
Affiliation(s)
- O Adriani
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - Y Akaike
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - M G Bagliesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - E Berti
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - G Bigongiari
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - W R Binns
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S Bonechi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - M Bongi
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - P Brogi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J H Buckley
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Castellini
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - C Checchia
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - M L Cherry
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Collazuol
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - V Di Felice
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - M Hareyama
- St. Marianna University School of Medicine, 2-16-1, Sugao, Miyamae-ku, Kawasaki, Kanagawa 216-8511, Japan
| | - N Hasebe
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Hibino
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - M Ichimura
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - K Ioka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwakecho, Sakyo, Kyoto 606-8502, Japan
| | - W Ishizaki
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - M H Israel
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - K Kasahara
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - J Kataoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - R Kataoka
- National Institute of Polar Research, 10-3, Midori-cho, Tachikawa, Tokyo 190-8518, Japan
| | - Y Katayose
- Faculty of Engineering, Division of Intelligent Systems Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - C Kato
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - N Kawanaka
- Hakubi Center, Kyoto University, Yoshida Honmachi, Sakyo-ku, Kyoto 606-8501, Japan
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Y Kawakubo
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Kohri
- Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan
| | - H S Krawczynski
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Lomtadze
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P Maestro
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P S Marrocchesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A M Messineo
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
- University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J W Mitchell
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Miyake
- Department of Electrical and Electronic Systems Engineering, National Institute of Technology, Ibaraki College, 866 Nakane, Hitachinaka, Ibaraki 312-8508 Japan
| | - A A Moiseev
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - K Mori
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - M Mori
- Department of Physical Sciences, College of Science and Engineering, Ritsumeikan University, Shiga 525-8577, Japan
| | - N Mori
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - H M Motz
- International Center for Science and Engineering Programs, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Munakata
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - H Murakami
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - S Nakahira
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - J Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - G A de Nolfo
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Okuno
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - J F Ormes
- Department of Physics and Astronomy, University of Denver, Physics Building, Room 211, 2112 East Wesley Avenue, Denver, Colorado 80208-6900, USA
| | - S Ozawa
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - L Pacini
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - F Palma
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - A V Penacchioni
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- ASI Science Data Center (ASDC), Via del Politecnico snc, 00133 Rome, Italy
| | - B F Rauch
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S B Ricciarini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - K Sakai
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Sakamoto
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - M Sasaki
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - Y Shimizu
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - A Shiomi
- College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino, Chiba 275-8575, Japan
| | - R Sparvoli
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Spillantini
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - F Stolzi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J E Suh
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A Sulaj
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - I Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8583, Japan
| | - M Takayanagi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - M Takita
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - T Tamura
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - N Tateyama
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - H Tomida
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Torii
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - Y Tsunesada
- Division of Mathematics and Physics, Graduate School of Science, Osaka City University, 3-3-138 Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
| | - Y Uchihori
- National Institutes for Quantum and Radiation Science and Technology, 4-9-1 Anagawa, Inage, Chiba 263-8555, Japan
| | - S Ueno
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - E Vannuccini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - J P Wefel
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Yamaoka
- Nagoya University, Furo, Chikusa, Nagoya 464-8601, Japan
| | - S Yanagita
- College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
| | - A Yoshida
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Yoshida
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| |
Collapse
|
43
|
Cholis I, Karwal T, Kamionkowski M. Features in the spectrum of cosmic-ray positrons from pulsars. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.123011] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
44
|
Cao J, Feng L, Guo X, Shang L, Wang F, Wu P. Scalar dark matter interpretation of the DAMPE data with U(1) gauge interactions. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.095011] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
45
|
Sui Y, Zhang Y. Prospects of type-II seesaw models at future colliders in light of the DAMPEe+e−excess. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.095002] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
46
|
Niu JS, Li T, Ding R, Zhu B, Xue HF, Wang Y. Bayesian analysis of the break in
DAMPE
lepton spectra. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.083012] [Citation(s) in RCA: 17] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
47
|
|