Constraints on WIMP Dark Matter from the High Energy PAMELA<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mover accent="true"><mml:mi>p</mml:mi><mml:mo>¯</mml:mo></mml:mover><mml:mo>/</mml:mo><mml:mi>p</mml:mi></mml:math>Data

Donato, Fiorenza; Maurin, D.; Brun, P.; Delahaye, Timur; Salati, Pierre

doi:10.1103/physrevlett.102.071301

Cited by 246 publications

(221 citation statements)

References 42 publications

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“…3 we also comment upon the consistency of these scenarios in the light of the new diffuse gamma ray data, as a specific application of the general constraints derived above. We limit ourselves to modes of annihilation in a pair of charged lepton final states at tree level since, on one hand, they appear the only ones not excluded by other constraints (most notably antiproton fraction [8,9]), on the other hand they are significantly less model-dependent than scenarios with annihilations proceeding via additional, non SM states [10]. For the case of decaying DM, which has been invoked as alternative explanation of the lepton anomalies, a fortiori we limit ourselves to leptonic channels.…”

Section: Introductionmentioning

confidence: 99%

Diffuse gamma ray constraints on annihilating or decaying Dark Matter after Fermi

Cirelli¹,

Panci²,

Serpico³

2010

Nuclear Physics B

201

246

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We consider the diffuse gamma ray data from Fermi first year observations and compare them to the gamma ray fluxes predicted by Dark Matter annihilation or decay (both from prompt emission and from Inverse Compton Scattering), for different observation regions of the sky and a range of Dark Matter masses, annihilation/decay channels and Dark Matter galactic profiles. We find that the data exclude large regions of the Dark Matter parameter space not constrained otherwise and discuss possible directions for future improvements. Also, we further constrain Dark Matter interpretations of the e ± PAMELA/Fermi spectral anomalies, both for the annihilating and the decaying Dark Matter case: under very conservative assumptions, only models producing dominantly µ ± and assuming a cored Dark Matter galactic profile can fit the lepton data with masses around ∼ 2 TeV.

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Section: Introductionmentioning

confidence: 99%

Diffuse gamma ray constraints on annihilating or decaying Dark Matter after Fermi

Cirelli¹,

Panci²,

Serpico³

2010

Nuclear Physics B

201

246

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“…The measured p/ p ratio is claimed to be a factor of 2 -3× larger than predicted by secondary cosmic-ray production models constrained by, for example, the positron fraction e + /(e + +e − ) and the B/C ratio [5]. Given the associated rising positron fraction [2] at 10 GeV, which is often explained as due to additional sources like pulsars, and not from enhanced cosmic-ray induced production, one may ask whether there is a consistent explanation for the overabundantp and the enhanced positron fraction.…”

Section: Introductionmentioning

confidence: 99%

“…First is that ratiosp/ p and e + /(e + + e − ) are far less useful than the particle spectral intensities themselves [37], particularly when looking at fits to data using models involving multiple source populations. Second is that the model [5] showing a discrepancy with the AMS-02 data, used to constrain fits for dark matter candidates top production, was tailored to fit PAMELA data that becomes increasingly uncertain at high energies.…”

Section: 6p/ P Ratiomentioning

confidence: 99%

Impact of Fermi-LAT and AMS-02 results on cosmic-ray astrophysics

Dermer

2015

EPJ Web of Conferences

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Abstract. This article reviews a few topics relevant to Galactic cosmic-ray astrophysics, focusing on the recent AMS-02 data release and Fermi Large Area Telescope data on the diffuse Galactic γ -ray emissivity. Calculations are made of the diffuse cosmic-ray induced p + p → π 0 → 2γ spectra, normalized to the AMS-02 cosmic-ray proton spectrum at ≈ 10 − 100 GV, with and without a hardening in the cosmic-ray proton spectrum at rigidities R 300 GV. A single power-law momentum "shock" spectrum for the local interstellar medium cosmic-ray proton spectrum cannot be ruled out from the γ -ray emissivity data alone without considering the additional contribution of electron bremsstrahlung. Metallicity corrections are discussed, and a maximal range of nuclear enhancement factors from 1.52 to 1.92 is estimated. Origins of the 300 GV cosmic-ray proton and α-particle hardening are discussed.

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“…Since no excess of antiprotons over what is expected from conventional astrophysics is evident, these measurements can be used to place bounds on properties of dark matter; this has been done in several earlier works (see, for instance, [6,13,14,15,16]). As an illustration of our results, we recalculate these bounds using the propagation model of Section 4.…”

Section: Effect On Pamela Constraintsmentioning

confidence: 99%

Antiprotons from dark matter: Effects of a position-dependent diffusion coefficient

Perelstein

Shakya

2011

Phys. Rev. D

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Energetic antiprotons in cosmic rays can serve as an important indirect signature of dark matter. Conventionally, the antiproton flux from dark matter decay or annihilation is calculated by solving the transport equation with a space-independent diffusion coefficient within the diffusion zone of the galaxy. Antiproton sources outside the diffusion zone are ignored under the assumption that they propagate freely and escape. In reality, it is far more likely that the diffusion coefficient increases smoothly with distance from the disk, and the outlying part of the dark matter halo ignored in the conventional approach can be significant, containing as much as 90% of the galactic dark matter by mass in some models. We extend the conventional approach to address these issues. We obtain analytic approximations and numerical solutions for antiproton flux for a diffusion coefficient that increases exponentially with the distance from the disk, thereby including contributions from dark matter annihilation/decay in essentially the full dark matter halo. We find that the antiproton flux predicted in this model deviates from the conventional calculation for the same dark matter parameters by up to about 25%.

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Constraints on WIMP Dark Matter from the High Energy PAMELAp¯/pData

Cited by 246 publications

References 42 publications

Diffuse gamma ray constraints on annihilating or decaying Dark Matter after Fermi

Diffuse gamma ray constraints on annihilating or decaying Dark Matter after Fermi

Impact of Fermi-LAT and AMS-02 results on cosmic-ray astrophysics

Antiprotons from dark matter: Effects of a position-dependent diffusion coefficient

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