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.
Highlights
The detectorThe DArk Matter Particle Explorer (DAMPE) is a satellite-born experiment and it is funded by the strategic space projects of the Chinese Academy of Sciences with the contribution of Italian and Swiss agencies [1, 2]
DAMPE (DArk Matter Particle Explorer) is a satellite-born experiment, resulting from the collaboration of Chinese, Italian, and Swiss institutions
The cosmic ray (CR) studies are based on the charge measurement, the STK tracking and the BGO imaging
Summary
The DArk Matter Particle Explorer (DAMPE) is a satellite-born experiment and it is funded by the strategic space projects of the Chinese Academy of Sciences with the contribution of Italian and Swiss agencies [1, 2]. It is devoted to measure the fluxes of charged cosmic rays (electrons, protons and heavier nuclei), to study the high energy gamma signal of astrophysical origin and to search for indirect dark matter signatures. The energy response to Minimum Ionizing Particles (MIPs), the efficiency and the detector alignment have been checked with a large sample of cosmic ray muon events. A similar plot is shown in the right panel of Fig. 4 for BGO signal due to helium nuclei not showering in the BGO calorimeter. In both cases the detector response is very stable
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