Gamma ray and neutrinos fluxes from a cosmological dark matter simulation

Athanassoula, E.; Ling, Fu-Sin; Nezri, E.; Teyssier, Romain

doi:10.1016/j.astropartphys.2008.11.002

Cited by 5 publications

(7 citation statements)

References 50 publications

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“…For the direction of the galactic center, BF is negligible if the halo is very cuspy. For a flat profile like the isothermal one, BF is also limited because the concentration of subhalos is comparable to that of the galactic halo [57]. On the particle physics side, the Sommerfeld effect can provide non negligible enhancements.…”

Section: γ and ν Signalsmentioning

confidence: 99%

Scalar multiplet dark matter

Hambye

Ling

Lopez-Honorez

et al. 2009

J. High Energy Phys.

263

333

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We perform a systematic study of the phenomenology associated to models where the dark matter consists in the neutral component of a scalar SU (2) L n-uplet, up to n = 7. If one includes only the pure gauge induced annihilation cross-sections it is known that such particles provide good dark matter candidates, leading to the observed dark matter relic abundance for a particular value of their mass around the TeV scale. We show that these values actually become ranges of values -which we determine -if one takes into account the annihilations induced by the various scalar couplings appearing in these models. This leads to predictions for both direct and indirect detection signatures as a function of the dark matter mass within these ranges. Both can be largely enhanced by the quartic coupling contributions. We also explain how, if one adds right-handed neutrinos to the scalar doublet case, the results of this analysis allow to have altogether a viable dark matter candidate, successful generation of neutrino masses, and leptogenesis in a particularly minimal way with all new physics at the TeV scale.

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Section: γ and ν Signalsmentioning

confidence: 99%

Scalar multiplet dark matter

Hambye

Ling

Lopez-Honorez

et al. 2009

J. High Energy Phys.

263

333

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“…Concerted theoretical and observational efforts are being made to detect the DM through photonic and leptonic signals [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19]. Extensions of the standard model of particle physics have been proposed to account for the observed anomalies in the PAMELA positron and FERMI electron plus positron data [4,5,7,9,10,[16][17][18].…”

Section: Introductionmentioning

confidence: 97%

“…The identity of dark matter (DM), which constitutes 23% of the total density of the Universe [1], has been one of the most important open questions in astrophysics for more than seven decades [2]. Concerted theoretical and observational efforts are being made to detect the DM through photonic and leptonic signals [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19]. Extensions of the standard model of particle physics have been proposed to account for the observed anomalies in the PAMELA positron and FERMI electron plus positron data [4,5,7,9,10,[16][17][18].…”

Section: Introductionmentioning

confidence: 99%

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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“…Often these results were derived from simulations that do not resolve the relevant subgalactic scales, and it is not clear that a simple extrapolation is justified, since not all substructure properties are scale-invariant. Some past work (Calcáneo-Roldán & Moore 2000;Stoehr et al 2003;Diemand et al 2006;Athanassoula et al 2008) has directly used numerical simulations, but these studies either suffered from insufficient resolution, did not correct for effects arising from the population of unresolved subhalos, or did not realistically account for the gammaray backgrounds against which individual subhalos must compete.…”

Section: Introductionmentioning

confidence: 98%

The Dark Matter Annihilation Signal from Galactic Substructure: Predictions forGLAST

Kuhlen

Diemand

Madau

2008

Astrophysical Journal

187

257

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We present quantitative predictions for the detectability of individual Galactic dark matter subhalos in gamma rays from dark matter pair annihilations in their centers. Our method is based on a hybrid approach, employing the highest resolution numerical simulations available (including the recently completed 1 billion particle Via Lactea II simulation), as well as analytical models, for extrapolating beyond the simulations' resolution limit. We include a selfconsistent treatment of subhalo boost factors, motivated by our numerical results, and a realistic treatment of the expected backgrounds that individual subhalos must outshine. We show that for reasonable values of the dark matter particle physics parameters (M $ 50Y500 GeV and hvi $ 10 À26 Y10 À25 cm 3 s À1 ) GLAST may very well discover a few, even up to several dozen, such subhalos at 5 significance, and some at more than 20 . We predict that the majority of luminous sources would be resolved with GLAST's expected angular resolution. For most observer locations, the angular distribution of detectable subhalos is consistent with a uniform distribution across the sky. The brightest subhalos tend to be massive (median V max of 24 km s À1 ) and therefore likely hosts of dwarf galaxies, but many subhalos with V max as low as 5 km s À1 are also visible. Typically detectable subhalos are 20Y40 kpc from the observer, and only a small fraction are closer than 10 kpc. The total number of observable subhalos has not yet converged in our simulations, and we estimate that we may be missing up to 3/4 of all detectable subhalos.

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Gamma ray and neutrinos fluxes from a cosmological dark matter simulation

Cited by 5 publications

References 50 publications

Scalar multiplet dark matter

Scalar multiplet dark matter

Probing dark matter models with neutrinos from the Galactic center

The Dark Matter Annihilation Signal from Galactic Substructure: Predictions forGLAST

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