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Constraining Dark Matter Properties with Gamma-Rays from the Galactic Center with Fermi-LAT
High Energy Astrophysical Phenomena · Submitted 2 Jun 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim If Fermi-LAT is able to distinguish a possible dark matter signal from the large gamma-ray background, we show that for dark matter masses below ~200 GeV, Fermi-LAT will likely be able to determine dark matter properties with good accuracy.
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The abstract, sentence by sentence
We study the capabilities of the Fermi-LAT instrument on board of the Fermi mission to constrain particle dark matter properties, as annihilation cross section, mass and branching ratio into dominant annihilation channels, with gamma-ray observations from the galactic center. Besides the prompt gamma-ray flux, we also take into account the contribution from the electrons/positrons produced in dark matter annihilations to the gamma-ray signal via inverse Compton scattering off the interstellar photon background, which turns out to be crucial in the case of dark matter annihilations into mu+mu- and e+e- pairs. We study the signal dependence on different parameters like the region of observation, the density profile, the assumptions for the dark matter model and the uncertainties in the propagation model. We also show the effect of the inclusion of a 20% systematic uncertainty in the gamma-ray background. If Fermi-LAT is able to distinguish a possible dark matter signal from the large gamma-ray background, we show that for dark matter masses below ~200 GeV, Fermi-LAT will likely be able to determine dark matter properties with good accuracy.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study the capabilities of the Fermi-LAT instrument on board of the Fermi mission to constrain particle dark matter properties, as annihilation cross section, mass and branching ratio into dominant annihilation channels, with gamma-ray observations from the galactic center. | contribution 0.98 | 0.84 | 0.07 | asserted 0.70 |
| s1 | Besides the prompt gamma-ray flux, we also take into account the contribution from the electrons/positrons produced in dark matter annihilations to the gamma-ray signal via inverse Compton scattering off the interstellar photon background, which turns out to be crucial in the case of dark matter annihilations into mu+mu- and e+e- pairs. | method 0.90 | 0.74 | 0.03 | asserted 0.99 |
| s2 | We study the signal dependence on different parameters like the region of observation, the density profile, the assumptions for the dark matter model and the uncertainties in the propagation model. | contribution 0.56 | 0.88 | 0.03 | asserted 0.93 |
| s3 | We also show the effect of the inclusion of a 20% systematic uncertainty in the gamma-ray background. | contribution 0.46 | 0.86 | 0.02 | asserted 0.96 |
| s4 | If Fermi-LAT is able to distinguish a possible dark matter signal from the large gamma-ray background, we show that for dark matter masses below ~200 GeV, Fermi-LAT will likely be able to determine dark matter properties with good accuracy. | result 0.66 | 0.81 | 0.81 | hedged possibility 0.99 |
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The paper
Original abstract
We study the capabilities of the Fermi-LAT instrument on board of the Fermi mission to constrain particle dark matter properties, as annihilation cross section, mass and branching ratio into dominant annihilation channels, with gamma-ray observations from the galactic center. Besides the prompt gamma-ray flux, we also take into account the contribution from the electrons/positrons produced in dark matter annihilations to the gamma-ray signal via inverse Compton scattering off the interstellar photon background, which turns out to be crucial in the case of dark matter annihilations into mu+mu- and e+e- pairs. We study the signal dependence on different parameters like the region of observation, the density profile, the assumptions for the dark matter model and the uncertainties in the propagation model. We also show the effect of the inclusion of a 20% systematic uncertainty in the gamma-ray background. If Fermi-LAT is able to distinguish a possible dark matter signal from the large gamma-ray background, we show that for dark matter masses below ~200 GeV, Fermi-LAT will likely be able to determine dark matter properties with good accuracy.
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References
How the literature uses it
18 arXiv papers cite this in 33 sentences
Papers citing it · 16 sentences without a confident label
Uses its method or tool 2 papers
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In order to calculate the ICS part we follow the tools and methods described in [ref] .
Galactic-Centre Gamma Rays in CMSSM Dark Matter Scenarios · The Inverse Compton Scattering component · 1.00
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However, let us note that Ref. [ref] makes use of the Fermi Science Tools, both to model the background and the signal.
Constraining the Milky Way Dark Matter Density Profile with Gamma-Rays with Fermi-LAT · Analysis · 0.93
Compares with it 1 paper
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On the other hand, the capabilities for the reconstruction of the DM mass and annihilation channel do not substantially worsen with respect to the case of a known DM density profile (but with a single angular bin) [ref] .
Constraining the Milky Way Dark Matter Density Profile with Gamma-Rays with Fermi-LAT · Constraining DM properties and the DM density profile · 1.00
Cites it as background 8 papers
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Indeed, several approaches have been proposed to determine DM particle properties by using future indirect WIMP DM-induced signals of gamma-rays or neutrinos, direct detection searches, collider information or their combination [ref] .
Constraining the Milky Way Dark Matter Density Profile with Gamma-Rays with Fermi-LAT · Conclusions · 0.87
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Again, the dependence on the propagation model has been studied in reference [ref] .
Reconstructing Dark Matter Properties via Gamma-Rays with Fermi-LAT · Introduction · 0.82
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This is now a hot theoretical [ref] and experimental topic, with several experiments [ref] studying the cosmic-ray $γ$ spectra from a variety of astrophysical sources such as the galactic centre and bulge as well as dwarf galaxies.
Galactic-Centre Gamma Rays in CMSSM Dark Matter Scenarios · Introduction · 0.95
What it cites · 139 sentences without a confident label
Builds on 4 papers
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As an improvement with respect to previous works [ref] , to the commonly considered gamma-ray prompt contribution, we add the contribution from the electrons and positrons produced in DM annihilations to the gamma-ray spectrum via inverse Compton scattering off the ambient photon background.
Extracting the Gamma Ray Signal from Dark Matter Annihilation in the Galactic Center Region · Introduction · 0.93
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As an improvement with respect to previous works [ref] , to the commonly considered gamma-ray prompt contribution, we add the contribution from the electrons and positrons produced in DM annihilations to the gamma-ray spectrum via inverse Compton scattering off the ambient photon background.
Determining the WIMP mass using the complementarity between direct and indirect searches and the ILC · Introduction · 0.93
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As an improvement with respect to previous works [ref] , to the commonly considered gamma-ray prompt contribution, we add the contribution from the electrons and positrons produced in DM annihilations to the gamma-ray spectrum via inverse Compton scattering off the ambient photon background.
WIMP mass from direct, indirect dark matter detection experiments and colliders: A complementary and model-independent approach · Introduction · 0.93
Uses the method or tool of 7 papers
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In this work we shall use the popular two-zone diffusion model and obtain the semi-analytical solution using the Bessel approach as described in detail in Ref. [ref] .
Positrons from dark matter annihilation in the galactic halo: theoretical uncertainties · Gamma–Rays from Inverse Compton Scattering · 1.00
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Following Ref. [ref] , we approximate the total radiation density as a superposition of three blackbody-like spectra,
Inverse Compton constraints on the Dark Matter e+e- excesses · Gamma–Rays from Inverse Compton Scattering · 0.98
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The treatment of this systematic error is performed by the Lagrange multiplier method or also so-called pull approach [ref] .
Uncertainties of Parton Distribution Functions and Their Implications on Physical Predictions · Dependence on systematic errors · 1.00
Uses data or values from 6 papers
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Recently the Fermi–LAT collaboration reported a new measurement of this high-energy gamma-ray emission [ref] , consistent with a power law with differential spectral index $α=2.41±0.05$ and intensity $Φ(E_γ>100$ MeV$)=(1.03±0.17)·10^-5$ cm$^-2$ s$^-1$ sr$^-1$ [ref] , i.e., for the best-fit values,
The Spectrum of the Isotropic Diffuse Gamma-Ray Emission Derived From First-Year Fermi Large Area Telescope Data · Isotropic Gamma-Ray Background · 0.99
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Regarding the propagation parameters $L$, $K_0$ and $α$, we take their values from the commonly used MIN, MAX and MED models [ref] (see Table [ref]), which correspond to the minimal, maximal and median primary positron fluxes over some energy range that are compatible with the B/C data [ref] .
Positrons from dark matter annihilation in the galactic halo: theoretical uncertainties · Gamma–Rays from Inverse Compton Scattering · 0.92
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Regarding the propagation parameters $L$, $K_0$ and $α$, we take their values from the commonly used MIN, MAX and MED models [ref] (see Table [ref]), which correspond to the minimal, maximal and median primary positron fluxes over some energy range that are compatible with the B/C data [ref] .
Cosmic Rays below Z=30 in a diffusion model: new constraints on propagation parameters · Gamma–Rays from Inverse Compton Scattering · 0.92
Compares with 6 papers
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Notice that Ref. [ref] (see also Ref. [ref] ) performed a similar analysis considering a region of $0.5^∘$ around the GC, which for a NFW density profile is expected to provide worse results by a factor of $∼$ 7–8 [ref] .
Fitting the Gamma-Ray Spectrum from Dark Matter with DMFIT: GLAST and the Galactic Center Region · Fermi–LAT sensitivity to DM annihilation · 1.00
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Notice that Ref. [ref] (see also Ref. [ref] ) performed a similar analysis considering a region of $0.5^∘$ around the GC, which for a NFW density profile is expected to provide worse results by a factor of $∼$ 7–8 [ref] .
Optimal angular window for observing Dark Matter annihilation from the Galactic Center region: the case of gamma-ray lines · Fermi–LAT sensitivity to DM annihilation · 1.00
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Notice that Ref. [ref] (see also Ref. [ref] ) performed a similar analysis considering a region of $0.5^∘$ around the GC, which for a NFW density profile is expected to provide worse results by a factor of $∼$ 7–8 [ref] .
Pre-launch estimates for GLAST sensitivity to Dark Matter annihilation signals · Fermi–LAT sensitivity to DM annihilation · 1.00
Cites as support 1 paper
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For the energies of interest here and for the observational regions we consider, this contribution is expected to be subdominant with respect to ICS [ref] , so for the sake of simplicity we do not discuss it any further.
Radio and gamma-ray constraints on dark matter annihilation in the Galactic center · Gamma–Rays from the Galactic Center · 0.96
Cites as background 83 papers
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The Fermi Gamma-ray Space Telescope (Fermi) [ref] was launched in June $2008$ for a mission of 5 to 10 years.
The Large Area Telescope on the Fermi Gamma-ray Space Telescope Mission · Fermi–LAT sensitivity to DM annihilation · 0.96
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Different approaches have been proposed to determine the DM properties by using indirect or direct measurements or their combination [ref] .
Annihilation vs. Decay: Constraining Dark Matter Properties from a Gamma-Ray Detection in Dwarf Galaxies · Introduction · 0.87
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Different approaches have been proposed to determine the DM properties by using indirect or direct measurements or their combination [ref] .
Determining the dark matter mass with DeepCore · Introduction · 0.87
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