Introduction. Vivre des déchets

Cirelli, Claudia; Florin, Bénédicte

doi:10.4000/books.pufr.7297

Cited by 6 publications

(9 citation statements)

References 25 publications

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“…If the WIMP was produced non-thermally in the early Universe (for example, from the decay of a heavier particle), it can naturally have a large annihilation crosssection [40,[61][62][63]. However, even if the WIMP was in thermal equilibrium in the early Universe, several mechanisms allow the cross-section to be large today while being much smaller at freeze-out [14][15][16][64][65][66][67][68]. The Sommerfeld enhancement [14][15][16][65][66][67][68] increases the crosssection at low dark matter velocities, v, so that the crosssection can be much larger today in the Milky-Way halo, where v ∼ 10 −3 , than during freeze-out, where v ∼ 0.3.…”

Section: Constraining Sommerfeld Enhanced Modelsmentioning

confidence: 99%

“…Constraints on dark matter annihilation to charged leptons are particularly relevant in light of the positron results from the PAMELA satellite in the energy range of 10-100 GeV [9] as well as the Fermi [10] and HESS [11,12] e + + e − spectra at ∼ 0.3 − 1 TeV. If dark matter annihilation is responsible for these measurements, the annihilation cross-section must be O(100 − 1000) times larger than the thermal freeze-out cross-section and only a small number of anti-protons can be created in the annihilation process [13][14][15][16][17][18][19][20]. Given the importance of the dark matter interpretation of these measurements, and the fact that more precise e + /e − flux measurements may not conclusively determine their origin (given the uncertainty in the e + /e − propagation in the Galaxy and in their background fluxes), independent checks of the dark matter interpretation of the PAMELA, Fermi, and HESS signals are of the utmost importance.…”

Section: Introductionmentioning

confidence: 99%

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Indirect dark matter detection limits from the ultrafaint Milky Way satellite Segue 1

et al. 2010

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We use new kinematic data from the ultra-faint Milky Way satellite Segue 1 to model its dark matter distribution and derive upper limits on the dark matter annihilation cross-section. Using gamma-ray flux upper limits from the Fermi satellite and MAGIC, we determine cross-section exclusion regions for dark matter annihilation into a variety of different particles including charged leptons. We show that these exclusion regions are beginning to probe the regions of interest for a dark matter interpretation of the electron and positron fluxes from PAMELA, Fermi, and HESS, and that future observations of Segue 1 have strong prospects for testing such an interpretation. We additionally discuss prospects for detecting annihilation with neutrinos using the IceCube detector, finding that in an optimistic scenario a few neutrino events may be detected. Finally we use the kinematic data to model the Segue 1 dark matter velocity dispersion and constrain Sommerfeld enhanced models.

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Section: Constraining Sommerfeld Enhanced Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Indirect dark matter detection limits from the ultrafaint Milky Way satellite Segue 1

et al. 2010

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“…It is possible for these excesses to be explained by conventional astrophysical objects such as nearby pulsars [10,11,12,13,14]. It is also possible that they may be the first indirect evidence of dark matter annihilations (e.g., [15,16,17,18,19,20,21,22,23,24,25,26,27,28,29,30,31,32,33,34,35,36,37,38,39,40]) or decays (e.g., [41,42,43,44,45,46,47,48,49,50,51]).…”

Section: Introductionmentioning

confidence: 99%

“…In light of the latter possibility, it has been shown that both PAMELA and ATIC/PPB-BETS, as well as a possible excess in microwave photons at the Galactic center dubbed the WMAP haze [52,53,54,55], may be explained by a ∼ 1 TeV dark matter particle which annihilates into charged leptons [15,16]. However, for this scenario to work, the annihilation cross-section in the Galactic halo must be boosted by factors of O(100) beyond the freeze-out cross-section.…”

Section: Introductionmentioning

confidence: 99%

“…However, for this scenario to work, the annihilation cross-section in the Galactic halo must be boosted by factors of O(100) beyond the freeze-out cross-section. One suggestion is that this could be achieved via a velocity dependent crosssection through the mechanism of Sommerfeld enhancement [16,17,56,57,58]. This idea supposes that the O(100) lower velocity dispersion in the Galactic halo as compared to the velocity at freeze-out could account for the necessary boost to explain these recent observations.…”

Section: Introductionmentioning

confidence: 99%

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Bounds on cross sections and lifetimes for dark matter annihilation and decay into charged leptons from gamma-ray observations of dwarf galaxies

2009

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We provide conservative bounds on the dark matter cross-section and lifetime from final state radiation produced by annihilation or decay into charged leptons, either directly or via an intermediate particle φ. Our analysis utilizes the experimental gamma-ray flux upper limits from four Milky Way dwarf satellites: HESS observations of Sagittarius and VERITAS observations of Draco, Ursa Minor, and Willman 1. Using 90% confidence level lower limits on the integrals over the dark matter distributions, we find that these constraints are largely unable to rule out dark matter annihilations or decays as an explanation of the PAMELA and ATIC/PPB-BETS excesses. However, if there is an additional Sommerfeld enhancement in dwarfs, which have a velocity dispersion ∼ 10 to 20 times lower than that of the local Galactic halo, then the cross-sections for dark matter annihilating through φ's required to explain the excesses are very close to the cross-section upper bounds from Willman 1. Dark matter annihilation directly into τ 's is also marginally ruled out by Willman 1 as an explanation of the excesses, and the required cross-section is only a factor of a few below the upper bound from Draco. Finally, we make predictions for the gamma-ray flux expected from the dwarf galaxy Segue 1 for the Fermi Gamma-ray Space Telescope. We find that for a sizeable fraction of the parameter space in which dark matter annihilation into charged leptons explains the PAMELA excess, Fermi has good prospects for detecting a gamma-ray signal from Segue 1 after one year of observation.

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Probing dark matter dynamics via earthborn neutrinos at IceCube

Delaunay

Fox

Pérez

2009

J. High Energy Phys.

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Recent results from PAMELA and ATIC hint that O(TeV) dark matter (DM) is annihilating, in our galactic neighborhood, predominantly to leptons. The annihilation rate is much larger now than during freeze-out, one possible explanation of this is a low-velocity enhancement of the annihilation cross section. In a model independent fashion, we show that in this case the rate of neutrino emission from the Earth, due to DM annihilation, may be greatly enhanced while the rate from the Sun is unaltered. There is potential for IceCube to see these earthborn neutrinos while the same parameter space will be soon covered by direct detection experiments. Combining these near-future data will allow extraction of valuable information about the DM sector dynamics.

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Introduction. Vivre des déchets

Cited by 6 publications

References 25 publications

Indirect dark matter detection limits from the ultrafaint Milky Way satellite Segue 1

Indirect dark matter detection limits from the ultrafaint Milky Way satellite Segue 1

Bounds on cross sections and lifetimes for dark matter annihilation and decay into charged leptons from gamma-ray observations of dwarf galaxies

Probing dark matter dynamics via earthborn neutrinos at IceCube

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