Dark Matter Particle Explorer observations of high-energy cosmic ray electrons plus positrons and their physical implications

Abstract

The DArk Matter Particle Explorer (DAMPE) is a satellite-borne, high-energy particle and γ-ray detector, which is dedicated to indirectly detecting particle dark matter and studying high-energy astrophysics. The first results about precise measurement of the cosmic ray electron plus positron spectrum between 25 GeV and 4.6 TeV were published recently. The DAMPE spectrum reveals an interesting spectral softening arount 0.9 TeV and a tentative peak around 1.4 TeV. These results have inspired extensive discussion. The detector of DAMPE, the data analysis, and the first results are introduced. In particular, the physical interpretations of the DAMPE data are reviewed. PACS numbers: 95.35.+d,95.85.Ry,96.50.sb * yuanq@pmo.ac.cn 1 See also earlier hints from HEAT and AMS measurements [16,17].

Indication of nearby source signatures of cosmic rays from energy spectra and anisotropies

“…This scenario should be natural. If SNRs are indeed the sources of GCRs, a simple estimate of SNRs in the local vicinity with proper distances and ages would lead to a number of a few, assuming a typical rate of Galactic supernovae [54]. We have added one additional source in the direction of (R.A.= 2 h 31 m , δ = −8 • 47 ′ ), with a distance of 300 pc and an age of 3 × 10 5 years in the model.…”

Machine learning-based method of calorimeter saturation correction for helium flux analysis with DAMPE experiment

“…Preliminary results on 𝛾-ray observations were also presented [16]. These studies show interesting spectral features which help to push our understanding of the CR astrophysics and constrain the dark matter models [17][18][19].…”

Recent status and results of the Dark Matter Particle Explorer

“…The wide energy range coverage and high precision of the DAMPE spectrum can significantly improve the constraints on the model parameters to fit the positron excess, either for astrophysical models or the DM annihilation or decay [27]. The spectral break may naturally reflect the discretness of the source distribution due to the fast cooling of TeV CREs [28]. Another interpretation ascribes the softening to the confinement and cooling of CREs during the acceleration stage [29].…”