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Inverse Compton gamma-rays from Galactic dark matter annihilation: Anisotropy signatures
High Energy Astrophysical Phenomena · Submitted 10 Aug 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Finally, the contribution from the smooth host halo component to the gamma-ray mean intensity is negligibly small compared to subhalos.
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
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The abstract, sentence by sentence
High energy electrons and positrons from annihilating dark matter can imprint unique angular anisotropies on the diffuse gamma-ray flux by inverse Compton scattering off the interstellar radiation field. We develop a numerical tool to compute gamma-ray emission from such electrons and positrons produced in the smooth host halo and in substructure halos with masses down to 10^(-6)M_sun. We show that the angular power spectrum from inverse Compton scattering is exponentially suppressed below an angular scale determined by the diffusion length of electrons and positrons. We also find that the total flux and the shape of the angular power spectrum depends sensitively on the spatial distribution of subhalos in the Milky Way. Finally, the contribution from the smooth host halo component to the gamma-ray mean intensity is negligibly small compared to subhalos.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | High energy electrons and positrons from annihilating dark matter can imprint unique angular anisotropies on the diffuse gamma-ray flux by inverse Compton scattering off the interstellar radiation field. | background 1.00 | 0.10 | 0.12 | hedged possibility 0.85 |
| s1 | We develop a numerical tool to compute gamma-ray emission from such electrons and positrons produced in the smooth host halo and in substructure halos with masses down to 10^(-6)M_sun. | method 0.83 | 0.96 | 0.05 | asserted 1.00 |
| s2 | We show that the angular power spectrum from inverse Compton scattering is exponentially suppressed below an angular scale determined by the diffusion length of electrons and positrons. | result 1.00 | 0.93 | 0.32 | asserted 1.00 |
| s3 | We also find that the total flux and the shape of the angular power spectrum depends sensitively on the spatial distribution of subhalos in the Milky Way. | result 1.00 | 0.96 | 0.20 | asserted 1.00 |
| s4 | Finally, the contribution from the smooth host halo component to the gamma-ray mean intensity is negligibly small compared to subhalos. | result 1.00 | 0.92 | 0.19 | asserted 1.00 |
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The paper
Original abstract
High energy electrons and positrons from annihilating dark matter can imprint unique angular anisotropies on the diffuse gamma-ray flux by inverse Compton scattering off the interstellar radiation field. We develop a numerical tool to compute gamma-ray emission from such electrons and positrons produced in the smooth host halo and in substructure halos with masses down to 10^(-6)M_sun. We show that the angular power spectrum from inverse Compton scattering is exponentially suppressed below an angular scale determined by the diffusion length of electrons and positrons. We also find that the total flux and the shape of the angular power spectrum depends sensitively on the spatial distribution of subhalos in the Milky Way. Finally, the contribution from the smooth host halo component to the gamma-ray mean intensity is negligibly small compared to subhalos.
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How the literature uses it
2 arXiv papers cite this in 2 sentences
What it cites · 56 sentences without a confident label
Builds on 6 papers
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The same numerical approach as in [ref] can be extended to the anisotropies from both the galactic and extragalactic dark matter contributions [ref] .
Robust identification of isotropic diffuse gamma rays from Galactic dark matter · Introduction · 0.82
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The same numerical approach as in [ref] can be extended to the anisotropies from both the galactic and extragalactic dark matter contributions [ref] .
The detectability of dark matter annihilation with Fermi using the anisotropy energy spectrum of the gamma-ray background · Introduction · 0.82
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The same numerical approach as in [ref] can be extended to the anisotropies from both the galactic and extragalactic dark matter contributions [ref] .
Extragalactic gamma-ray background radiation from dark matter annihilation · Introduction · 0.82
Uses the method or tool of 6 papers
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The line-of-sight integral can directly act on the free Green's function [ref] , [equation] where we have defined the unit-vector $n≡r/ℓ$.
Diffuse inverse Compton and synchrotron emission from dark matter annihilations in galactic satellites · Green's function · 1.00
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Alternatively, for primary electrons and positrons from the smooth host dark matter halo, the Bessel-Fourier scheme [ref] can require less computational time than the Green's function.
Positrons from dark matter annihilation in the galactic halo: theoretical uncertainties · Halo function · 0.96
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Alternatively, for primary electrons and positrons from the smooth host dark matter halo, the Bessel-Fourier scheme [ref] can require less computational time than the Green's function.
Cosmic Rays below Z=30 in a diffusion model: new constraints on propagation parameters · Halo function · 0.96
Uses data or values from 4 papers
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Therefore, here we use the Einasto profile with the parameter $α=0.16$ given by Gao et al [ref] , [equation] The relation of halo concentration and mass is given by [equation] The slope and normalization are consistent with those found by Bullock et al [ref] .
The redshift dependence of the structure of massive LCDM halos · The subhalo density profile · 0.80
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Therefore, here we use the Einasto profile with the parameter $α=0.16$ given by Gao et al [ref] , [equation] The relation of halo concentration and mass is given by [equation] The slope and normalization are consistent with those found by Bullock et al [ref] .
Profiles of dark haloes: evolution, scatter, and environment · The subhalo density profile · 0.80
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For a host halo with the NFW density profile we adopted $ρ_s=0.2 GeV/cm^3$, $r_s=21.7$kpc and $c_200=12$ [ref] .
Neutralino annihilation into gamma-rays in the Milky Way and in external galaxies · Subhalo radial distribution · 0.90
Compares with 2 papers
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Empirically, we find that the mean intensity roughly doubles with each decade of decreasing mass of subhalos, similar to what has been found by Ref. [ref] .
Revealing dark matter substructure with anisotropies in the diffuse gamma-ray background · Diffuse Gamma-ray Emission · 0.95
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We also verified that the deviation from the detailed numerical simulation with Galprop [ref] is less than a factor of two for a realistic spatial distribution of the ISRF [ref] .
Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field · Energy losses · 0.87
Cites as background 16 papers
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The first calculations of this kind were performed analytically for gamma-ray background anisotropies induced by both annihilating extragalactic dark matter halos [ref] as well as Galactic subhalos [ref] .
Anisotropy of the cosmic gamma-ray background from dark matter annihilation · Introduction · 0.90
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The first calculations of this kind were performed analytically for gamma-ray background anisotropies induced by both annihilating extragalactic dark matter halos [ref] as well as Galactic subhalos [ref] .
Gamma-ray background anisotropy from galactic dark matter substructure · Introduction · 0.90
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The first calculations of this kind were performed analytically for gamma-ray background anisotropies induced by both annihilating extragalactic dark matter halos [ref] as well as Galactic subhalos [ref] .
Dark matter annihilation or unresolved astrophysical sources? Anisotropy probe of the origin of cosmic gamma-ray background · Introduction · 0.90
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