Antiproton identification below threshold with the AMS-02 RICH detector

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Zi-Yuan Li, Carlos Jose Delgado Mendez, Francesca Giovacchini, Sadakazu Haino and Julia Hoffman. Antiproton identification below threshold with the AMS-02 RICH detector[J]. Chinese Physics C, 2017, 41(5): 056001. doi: 10.1088/1674-1137/41/5/056001
Zi-Yuan Li, Carlos Jose Delgado Mendez, Francesca Giovacchini, Sadakazu Haino and Julia Hoffman. Antiproton identification below threshold with the AMS-02 RICH detector[J]. Chinese Physics C, 2017, 41(5): 056001.  doi: 10.1088/1674-1137/41/5/056001 shu
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Received: 2016-11-08
Revised: 2016-12-29
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    Supported by China Scholarship Council (CSC) under Grant No.201306380027.

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Antiproton identification below threshold with the AMS-02 RICH detector

    Corresponding author: Zi-Yuan Li,
  • 1. School of Physics, Sun Yat-Sen University, Guangdong 510275, China
  • 2. Institute of Physics, Academia Sinica, Taipei 11529, China
  • 3.  Centro de Investigaciones Energeticas, Mediambientales y Tecnologicas (CIEMAT), Madrid E-28040, Spain
  • 4.  Institute of Physics, Academia Sinica, Taipei 11529, China
  • 5.  Physics and Astronomy Department, University of Hawaii, Hawaii 96822, USA
Fund Project:  Supported by China Scholarship Council (CSC) under Grant No.201306380027.

Abstract: The Alpha Magnetic Spectrometer (AMS-02), which is installed on the International Space Station (ISS), has been collecting data successfully since May 2011. The main goals of AMS-02 are the search for cosmic anti-matter, dark matter and the precise measurement of the relative abundance of elements and isotopes in galactic cosmic rays. In order to identify particle properties, AMS-02 includes several specialized sub-detectors. Among these, the AMS-02 Ring Imaging Cherenkov detector (RICH) is designed to provide a very precise measurement of the velocity and electric charge of particles. We describe a method to reject the dominant electron background in antiproton identification with the use of the AMS-02 RICH detector as a veto for rigidities below 3 GV. A ray tracing integration method is used to maximize the statistics of p with the lowest possible e- background, providing 4 times rejection power gain for e- background with respect to only 3% of p signal efficiency loss. By using the collected cosmic-ray data, e- contamination can be well suppressed within 3% with β ≈ 1, while keeping 76% efficiency for p below the threshold.

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