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Galactic Center Excess

After introducing some general features of such dark matter agents, we introduce a set of established models which guide us through four experimental aspects: the dark matter relic density extracted from the cosmic microwave background, indirect detection including the Fermi galactic center excess, direct detection, and collider searches.

Yet Another Introduction to Dark Matter: The Particle Physics Approach

Galactic Center Excess

There is growing evidence that the Galactic Center Excess identified in the $\textit{Fermi}$-LAT gamma-ray data arises from a population of faint astrophysical sources.

Strong Evidence that the Galactic Bulge is Shining in Gamma Rays

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10.1007/978-3-030-16234-4

After introducing some general features of such dark matter agents, we introduce a set of established models which guide us through four experimental aspects: the dark matter relic density extracted from the cosmic microwave background, indirect detection including the Fermi galactic center excess, direct detection, and collider searches.

Yet Another Introduction to Dark Matter: The Particle Physics Approach

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10.1088/1475-7516/2019/09/042

There is growing evidence that the Galactic Center Excess identified in the $\textit{Fermi}$-LAT gamma-ray data arises from a population of faint astrophysical sources.

Strong Evidence that the Galactic Bulge is Shining in Gamma Rays

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10.1007/JHEP11(2019)048

We further show the parameter space which provides a good fit to the Galactic center excess data and is compatible with the current bounds and LUX-ZEPLIN projected sensitivity.

Thermodynamic Evolution of Secluded Vector Dark Matter: Conventional WIMPs and Nonconventional WIMPs

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10.1007/JHEP05(2020)081

Specifically the dark matter models favored by the Fermi Galactic center excess is expected to be detected or constrained at the 5(3) −σ level assuming a optimistic (conservative) propagation model.

Searching for dark photon dark matter with cosmic ray antideuterons

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10.1103/PhysRevD.99.123027

For models where the DM substructures have masses above $10^{-6}$ solar masses our limits probe the DM interpretation of the Fermi LAT Galactic center excess.

Search for γ -ray emission from dark matter particle interactions from the Andromeda and Triangulum galaxies with the Fermi Large Area Telescope

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10.1103/PhysRevD.100.055002

Our study is of special relevance in view of a recent analysis that casts doubt on the previously accepted preference for mili-second pulsars as the origin of the galactic center excess.

Return of the WIMP: Missing energy signals and the Galactic Center excess

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10.22323/1.364.0099

Recent (and earlier) analyses of the data from Planck, Fermi-LAT, AMS-02, and other experiments indicate that (i) the positron excess at ∼ 800 GeV or above is not evidence of highmass dark matter particles (which would have disconfirmed the present theory with a rigorous upper limit of 125 GeV), (ii) the Galactic center excess of gamma rays observed by Fermi is evidence for dark matter particles with a mass below or near 100 GeV, (iii) the gamma-ray excess from Omega Centauri is similar evidence of annihilation of such relatively low-mass particles, and (iv) the antiproton excess observed by AMS is again evidence of.

P 2 0 1 9 ) 0 9 9 A multicomponent dark matter scenario and the experimental evidence supporting it

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Center Excess - After introducing some general features of such dark matter agents, we introduce a set of established models which guide us through four experimental aspects: the dark matter relic density extracted from the cosmic microwave background, indirect detection including the Fermi galactic center excess, direct detection, and collider searches. [1] There is growing evidence that the Galactic Center Excess identified in the $\textit{Fermi}$-LAT gamma-ray data arises from a population of faint astrophysical sources. [2] We further show the parameter space which provides a good fit to the Galactic center excess data and is compatible with the current bounds and LUX-ZEPLIN projected sensitivity. [3] Specifically the dark matter models favored by the Fermi Galactic center excess is expected to be detected or constrained at the 5(3) −σ level assuming a optimistic (conservative) propagation model. [4] For models where the DM substructures have masses above $10^{-6}$ solar masses our limits probe the DM interpretation of the Fermi LAT Galactic center excess. [5] Our study is of special relevance in view of a recent analysis that casts doubt on the previously accepted preference for mili-second pulsars as the origin of the galactic center excess. [6] Recent (and earlier) analyses of the data from Planck, Fermi-LAT, AMS-02, and other experiments indicate that (i) the positron excess at ∼ 800 GeV or above is not evidence of highmass dark matter particles (which would have disconfirmed the present theory with a rigorous upper limit of 125 GeV), (ii) the Galactic center excess of gamma rays observed by Fermi is evidence for dark matter particles with a mass below or near 100 GeV, (iii) the gamma-ray excess from Omega Centauri is similar evidence of annihilation of such relatively low-mass particles, and (iv) the antiproton excess observed by AMS is again evidence of. [7]

Galactic Center Excess

After introducing some general features of such dark matter agents, we introduce a set of established models which guide us through four experimental aspects: the dark matter relic density extracted from the cosmic microwave background, indirect detection including the Fermi galactic center excess, direct detection, and collider searches. [1] There is growing evidence that the Galactic Center Excess identified in the $\textit{Fermi}$-LAT gamma-ray data arises from a population of faint astrophysical sources. [2] We further show the parameter space which provides a good fit to the Galactic center excess data and is compatible with the current bounds and LUX-ZEPLIN projected sensitivity. [3] Specifically the dark matter models favored by the Fermi Galactic center excess is expected to be detected or constrained at the 5(3) −σ level assuming a optimistic (conservative) propagation model. [4] For models where the DM substructures have masses above $10^{-6}$ solar masses our limits probe the DM interpretation of the Fermi LAT Galactic center excess. [5] Our study is of special relevance in view of a recent analysis that casts doubt on the previously accepted preference for mili-second pulsars as the origin of the galactic center excess. [6] Recent (and earlier) analyses of the data from Planck, Fermi-LAT, AMS-02, and other experiments indicate that (i) the positron excess at ∼ 800 GeV or above is not evidence of highmass dark matter particles (which would have disconfirmed the present theory with a rigorous upper limit of 125 GeV), (ii) the Galactic center excess of gamma rays observed by Fermi is evidence for dark matter particles with a mass below or near 100 GeV, (iii) the gamma-ray excess from Omega Centauri is similar evidence of annihilation of such relatively low-mass particles, and (iv) the antiproton excess observed by AMS is again evidence of. [7]