Upper limits on dark matter annihilation with the teraelectronvolt cosmic ray spectrum of electrons and positrons from DAMPE

Abstract

We have used teraelectronvolt cosmic ray spectrum of electrons and positrons data from DArk Matter Particle Explorer (DAMPE) to estimate the upper limits on dark matter annihilation. We have created modeled spectrum of electrons and positrons by considering dark matter annihilation into electrons and positrons with different channels. After the production, electrons and positrons can lose their energy by interstellar medium and interstellar radiation field. We have considered loss processes such as inverse Compton scattering, synchrotron radiation and ionization. The upper limits on dark matter annihilation cross-section have been investigated by comparing the model spectrum and observational spectrum. The stringent constraints is from electron-positron channel.

Status, Challenges and Directions in Indirect Dark Matter Searches

“…Indirect searches for dark matter have indeed been performed by gamma-ray telescopes (MAGIC, e.g., [84][85][86], H.E.S.S., e.g., [87][88][89][90], VERITAS [91,92]), X-ray telescopes (XMM-Newton, e.g., [93][94][95][96], NuSTAR, e.g., [97][98][99], Suzaku, e.g., [100][101][102][103]), cosmic-ray detectors (HAWC [104][105][106]), detectors in space (Fermi-LAT, e.g., [107][108][109], DAMPE, e.g., [110], CALET [111], AMS [112]) and neutrino telescopes (IceCube, e.g., [113][114][115], ANTARES, e.g., [116][117][118], Baikal, e.g., [119][120][121], Baksan [122] or Super-Kamiokande, e.g., [123][124][125]). Many of these detectors have upgrade programs underway, in different stages of R&D or implementation (CTA [126], IceCube-Gen2 [127], KM3NET [128]<...>…”

“…[70][71][72], DAMPE, e.g. [73], CALET [74], AMS [75]) and neutrino telescopes (IceCube, e.g. [76][77][78], ANTARES, e.g.…”