Prospects of detecting dark matter through cosmic-ray antihelium with the antiproton constraints

Cosmic-ray (CR) antihelium is an important observable for dark matter (DM) indirect searches due to extremely low secondary backgrounds towards low energies. In a given DM model, the predicted CR antihelium flux is expected to be strongly correlated with that of CR antiprotons. In this work, we use...

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Bibliographic Details
Published inJournal of cosmology and astroparticle physics Vol. 2019; no. 6; p. 4
Main Authors Ding, Yu-Chen, Li, Nan, Wei, Chun-Cheng, Wu, Yue-Liang, Zhou, Yu-Feng
Format Journal Article
LanguageEnglish
Published Bristol IOP Publishing 03.06.2019
Subjects
Antiparticles
Antiprotons
Coalescence
Coalescing
Computer simulation
Cosmic rays
Cross-sections
Dark matter
Generators
Kinetic energy
Monte Carlo simulation
Uncertainty analysis
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Summary:Cosmic-ray (CR) antihelium is an important observable for dark matter (DM) indirect searches due to extremely low secondary backgrounds towards low energies. In a given DM model, the predicted CR antihelium flux is expected to be strongly correlated with that of CR antiprotons. In this work, we use the AMS-02 /p data to constrain the DM annihilation cross section, and the ALICE data on the 3 and productions to determine the parameters in the coalescence model for anti-nucleus formation. The hadronic cross sections are estimated using Monte-Carlo event generators including EPOS-LHC and DPMJET. Based on these constraints, we make predictions for the maximal antihelium flux for typical DM annihilation final states, and perform a detailed analysis on the uncertainties due to the DM density profiles and CR propagation models. We find that the results are highly insensitive to both of them, but still significantly depend on the hadronization models in event generators. The prospects of detecting antihelium for the AMS-02 experiment is discussed. We show that with very optimistic assumptions, CR 3 is within the reach of the AMS-02 experiment. The 3 events which can be detected by AMS-02 are likely to have kinetic energy T≳30 GeV, which is consistent with the preliminary AMS-02 search results. The events which can be observed by AMS-02 are likely to arise dominantly from secondary backgrounds rather than DM interactions.
ISSN:1475-7516
1475-7516
DOI:10.1088/1475-7516/2019/06/004