Muon fluxes and showers from dark matter annihilation in the Galactic center

Erkoca, Arif Emre; Gelmini, Graciela B.; Reno, Mary Hall; Sarčević, Ina

doi:10.1103/physrevd.81.096007

Cited by 12 publications

(17 citation statements)

References 76 publications

(77 reference statements)

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“…For annihilation directly to neutrinos, the energy distribution of each neutrino is a delta function in energy, with the energy equal to the DM mass. This case has been well studied in the literature [21,31,32,36]. Here, we look at the secondary neutrinos.…”

Section: Models For Dark Mattermentioning

confidence: 93%

“…We show that for each model, the shape of the muon and shower fluxes differs significantly from the shape of the neutrino fluxes at production due to the smearing produced by neutrino interactions and muon propagation as discussed in Refs. [31,32]. We also calculate the detection significances of the DM signals at the IceCube/DeepCore [28] detector and compare the different DM models in terms of the energy spectra and the total counts of the muon and shower events.…”

Section: Introductionmentioning

confidence: 99%

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Probing dark matter models with neutrinos from the Galactic center

2010

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We calculate the contained and upward muon and shower fluxes due to neutrinos produced via dark matter annihilation or decay in the Galactic center. We consider dark matter models in which the dark matter particle is a gravitino, a Kaluza-Klein particle and a particle in leptophilic models. The Navarro-Frenk-White profile for the dark matter density distribution in the Galaxy is used. We incorporate neutrino oscillations by assuming maximal mixing and parametrize our results for muon and shower distributions. The muon and shower event rates and the minimum observation times in order to reach 2$\sigma$ detection significance are evaluated. We illustrate how observation times vary with the cone half angle chosen about the Galactic center, with the result that the optimum angles are about 10$^\circ$ and 50$^\circ$ for the muon events and shower events, respectively. We find that for the annihilating dark matter models such as the leptophilic and Kaluza-Klein models, upward and contained muon as well as showers are promising signals for dark matter detection in just a few years of observation, whereas for decaying dark matter models, the same observation times can only be reached with showers. We also illustrate for each model the parameter space probed with the 2$\sigma$ signal detection in five years. We discuss how the shape of the parameter space probed change with significance and the observation time.Comment: 19 pages, 20 figures, 9 tables. v2: summary table added, minor typos corrected, version accepted for publication in Phys. Rev.

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Section: Models For Dark Mattermentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Probing dark matter models with neutrinos from the Galactic center

2010

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“…Ref. [50] converts the SuperK limits into an upper limit on the annihilation cross section to a neutrino-antineutrino pair. Comparing this with limits on the same channel from Ref.…”

Section: Neutrinosmentioning

confidence: 99%

Dark matter annihilation signatures from electroweak bremsstrahlung

et al. 2011

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We examine observational signatures of dark matter annihilation in the Milky Way arising from electroweak bremsstrahlung contributions to the annihilation cross section. It has been known for some time that photon bremsstrahlung may significantly boost DM annihilation yields. Recently, we have shown that electroweak bremsstrahlung of W and Z gauge bosons can be the dominant annihilation channel in some popular models with helicity-suppressed 2 → 2 annihilation. W /Z-bremsstrahlung is particularly interesting because the gauge bosons produced via annihilation subsequently decay to produce large correlated fluxes of electrons, positrons, neutrinos, hadrons (including antiprotons) and gamma rays, which are all of importance in indirect dark matter searches. Here we calculate the spectra of stable annihilation products produced via γ/W /Z-bremsstrahlung. After modifying the fluxes to account for the propagation through the Galaxy, we set upper bounds on the annihilation cross section via a comparison with observational data. We show that stringent cosmic ray antiproton limits preclude a sizable dark matter contribution to observed cosmic ray positron fluxes in the class of models for which the bremsstrahlung processes dominate.PACS numbers: 95.35.+d, 12.15.Lk, 95.85.Ry

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“…We present the neutrino maps in Mollweide projection using HEALPix [134]. extrapolating to higher energies with a spectral power law of 3.7 for the differential spectrum [40].…”

Section: Exciting Dark Matter Annihilation Connecting To the Fermentioning

confidence: 99%

“…Measurements of CRs [16][17][18][19][20][21][22] have generated new model building [8,[23][24][25][26][27][28][29][30][31][32][33][34] and have helped place new constraints on dark matter properties [35][36][37][38][39]. Since many of these models and constraints are placed at the TeV mass scale and suggest or refer to enhanced (boosted) annihilation cross sections with hard spectra for the Standard Model (SM) particle annihilation products, neutrino signals from the galactic center (GC) [40] from the Sun [41] or the Earth [42] can be considered of interest.…”

Section: Introductionmentioning

confidence: 99%

Searching for the high-energy neutrino counterpart signals: The case of the Fermi bubbles signal and of dark matter annihilation in the inner Galaxy

Cholis

2013

Phys. Rev. D

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The recent uncovering of the Fermi bubbles/haze in the Fermi -ray data has generated theoretical work to explain such a signal of hard rays in combination with the WMAP haze signal. Many of these theoretical models can have distinctively different implications with regards to the production of highenergy neutrinos. We discuss the neutrino signals from different models proposed for the explanation of the Fermi bubbles/haze, more explicitly, from dark matter annihilation in the galactic halo with conditions of preferential cosmic ray diffusion, from recent active galactic nucleus jet activity, from periodic diffusive shock acceleration, from stochastic second order Fermi acceleration and from long time-scale star formation in the galactic center in combination with strong galactic winds. We find that some of these models will be probed by the IceCube DeepCore detector. Moreover, with a km 3 telescope located in the Northern Hemisphere, we will be able to discriminate between the hadronic, leptonic and the dark matter models. Additionally using the reconstructed neutrino spectra we will probe annihilation of TeV scale dark matter towards the galactic center.

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Muon fluxes and showers from dark matter annihilation in the Galactic center

Cited by 12 publications

References 76 publications

Probing dark matter models with neutrinos from the Galactic center

Probing dark matter models with neutrinos from the Galactic center

Dark matter annihilation signatures from electroweak bremsstrahlung

Searching for the high-energy neutrino counterpart signals: The case of the Fermi bubbles signal and of dark matter annihilation in the inner Galaxy

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