Revisit of cosmic ray antiprotons from dark matter annihilation with updated constraints on the background model from AMS-02 and collider data

Cui, Ming-Yang; Xu, Pan; Yuan, Qiang; Fan, Yi-Zhong; Zong, Hong-Shi

doi:10.1088/1475-7516/2018/06/024

Cited by 39 publications

(49 citation statements)

References 91 publications

(147 reference statements)

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“…Intriguingly, DM masses of about 60 GeV best fit the GCE, and as mentioned above, are consistent with the ones that lead to an explanation of the LHC tri-lepton signatures. Moreover, a recent excess in antiprotons observed by the AMS-02 experiment [30] seems to be consistent with DM annihilating into bottom-quark pairs, with a similar range of DM masses, and for annihilation cross sections consistent with the ones necessary to explain the GCE [31][32][33][34][35]. In view of all the above, it seems highly relevant to investigate extensions of our previous work [7] that, without changing the main results allowing for the interpretation of a possible LHC excess in the ATLAs tri-lepton plus missing energy signal, could lead to a DM explanation of the GCE (as well as the anti-proton excess observed by AMS-02).…”

Section: Introductionmentioning

confidence: 63%

Return of the WIMP: Missing energy signals and the Galactic Center excess

et al. 2019

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In a recent work, we emphasized that an excess in tri-lepton events plus missing energy observed by the ATLAS experiment at the LHC could be interpreted as a signal of low energy supersymmetry. In such a scenario the lightest neutralino mass is approximately m χ ≃ 60 GeV and the direct Dark Matter detection cross section is naturally below the current bound. In this work we present simple extensions of this scenario that lead to an explanation of the gamma ray excess at the center of the galaxy observed by Fermi-LAT, as well as the anti-proton excess observed by AMS-02. These extensions include the addition of a small CP violating phase in the neutralino sector or the addition of a light CP-odd Higgs scalar. Our study is of special relevance in view of a recent analysis that casts doubt on the previously accepted preference for mili-second pulsars as the origin of the galactic center excess.

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Section: Introductionmentioning

confidence: 63%

Return of the WIMP: Missing energy signals and the Galactic Center excess

et al. 2019

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“…Antimatter in cosmic rays (CRs), and in particular antiprotons, have been extensively investigated as a powerful means to search for exotic CR sources, such as dark matter (DM) annihilation in the Galaxy [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16]. The recent very accurate measurement of the CR antiproton flux by the AMS-02 experiment [17] has significantly increased the sensitivity to a DM signal.…”

Section: Introductionmentioning

confidence: 99%

Scrutinizing the evidence for dark matter in cosmic-ray antiprotons

et al. 2019

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Global fits of primary and secondary cosmic-ray (CR) fluxes measured by AMS-02 have great potential to study CR propagation models and search for exotic sources of antimatter such as annihilating dark matter (DM). Previous studies of AMS-02 antiprotons revealed a possible hint for a DM signal which, however, could be affected by systematic uncertainties. To test the robustness of such a DM signal, in this work we systematically study two important sources of uncertainties: the antiproton production cross sections needed to calculate the source spectra of secondary antiprotons and the potential correlations in the experimental data, so far not provided by the AMS-02 Collaboration. To investigate the impact of cross-section uncertainties we perform global fits of CR spectra including a covariance matrix determined from nuclear cross-section measurements. As an alternative approach, we perform a joint fit to both the CR and cross-section data. The two methods agree and show that cross-section uncertainties have a small effect on the CR fits and on the significance of a potential DM signal, which we find to be at the level of 3σ. Correlations in the data can have a much larger impact. To illustrate this effect, we determine possible benchmark models for the correlations in a data-driven method. The inclusion of correlations strongly improves the constraints on the propagation model and, furthermore, enhances the significance of the DM signal up to above 5σ. Our analysis demonstrates the importance of providing the covariance of the experimental data, which is needed to fully exploit their potential.

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“…The annihilation of DM particles in our galaxy as well as in extra-galactic objects leads to gamma-ray signals [15][16][17][18][19][20][21] as well as positrons, antiprotons etc [22][23][24][25]. Constraints have been imposed on DM annihilation rates in various ways out of the (non)-observation of such signals [26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

Heavy dark matter particle annihilation in dwarf spheroidal galaxies: Radio signals at the SKA telescope

Kar

Mitra²,

Mukhopadhyaya

et al. 2020

Phys. Rev. D

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A weakly interacting dark matter candidate is very difficult to detect at highenergy colliders like the LHC, if its mass is close to, or higher than, a TeV. We argue that the pair-annihilation of such particles may give rise to e + e − -pairs in dwarf spheroidal galaxies (dSph), which in turn can lead to radio synchrotron signals that are detectable at the upcoming square kilometre array (SKA) telescope within a fairly moderate observation time. We investigate in detail the underlying mechanisms that make this possible. Both particle physics issues and those pertaining to astrophysics, such as diffusion, electromagnetic energy loss and the effects of interstellar magnetic field, are examined with reference to their roles in generating radio flux. We first identify the detectability criteria in a model-independent manner. It is observed that fluxes may be detectable for scenarios that are consistent with all constraints available till date from γ-ray and cosmic-ray observations. Thereafter, using benchmarks based on popular scenarios involving physics beyond the standard model, we show that it should be possible to detect the radio flux from a dSph like Draco with 100 hours of observation at the SKA, for dark matter particle masses upto 4-8 TeV. The corresponding frequency distributions are also presented, where it is found that the frequency range 300 MHz -50 GHz is especially useful for recording the annihilation signals of trans-TeV particles.

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Revisit of cosmic ray antiprotons from dark matter annihilation with updated constraints on the background model from AMS-02 and collider data

Cited by 39 publications

References 91 publications

Return of the WIMP: Missing energy signals and the Galactic Center excess

Return of the WIMP: Missing energy signals and the Galactic Center excess

Scrutinizing the evidence for dark matter in cosmic-ray antiprotons

Heavy dark matter particle annihilation in dwarf spheroidal galaxies: Radio signals at the SKA telescope

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