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Spin-one dark matter and gamma ray signals from the galactic center
High Energy Physics - Phenomenology · Submitted 5 Nov 2019
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Taking into account all these contributions, our results for photons produced in the annihilation of SODM are in good agreement with the GRE data for $g_{s}\in [0.98, 1.01] \times 10^{-3}$ and $M\in [62.470,62.505]~GeV$.
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The abstract, sentence by sentence
In this work we study the possibility that the gamma ray excess (GRE) at the Milky Way galactic center come from the annihilation of dark matter with a $(1,0)\oplus(0,1)$ space-time structure (spin-one dark matter, SODM). We calculate the production of prompt photons from initial state radiation, internal bremsstrahlung, final state radiation including the emission from the decay products of the $\mu, \tau$ or hadronization of quarks. Next we study the delayed photon emission from the inverse Compton scattering (ICS) of electrons (produced directly or in the prompt decay of $\mu, \tau$ leptons or in the hadronization of quarks produced in the annihilation of SODM) with the cosmic microwave background or starlight. All these mechanisms yield significant contributions only for Higgs resonant exchange, i.e. for $M\approx M_{H}/2$, and the results depend on the Higgs scalar coupling to SODM, $g_{s}$. The dominant mechanism at the GRE bump is the prompt photon production in the hadronization of $b$ quarks produced in $\bar{D}D\to \bar{b}b$, whereas the delayed photon emission from the ICS of electrons coming from the hadronization of $b$ quarks produced in the same reaction dominates at low energies ($\omega < 0.3~ GeV$) and prompt photons from $c$ and $\tau$, as well as from internal bremsstrahlung, yield competitive contributions at the end point of the spectrum ($\omega \ge 30 ~GeV$). Taking into account all these contributions, our results for photons produced in the annihilation of SODM are in good agreement with the GRE data for $g_{s}\in [0.98, 1.01] \times 10^{-3}$ and $M\in [62.470,62.505]~GeV$.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In this work we study the possibility that the gamma ray excess (GRE) at the Milky Way galactic center come from the annihilation of dark matter with a $(1,0)\oplus(0,1)$ space-time structure (spin-one dark matter, SODM). | contribution 0.98 | 0.75 | 0.07 | hedged possibility 0.94 |
| s1 | We calculate the production of prompt photons from initial state radiation, internal bremsstrahlung, final state radiation including the emission from the decay products of the $\mu, \tau$ or hadronization of quarks. | method 0.89 | 0.94 | 0.02 | asserted 0.94 |
| s2 | Next we study the delayed photon emission from the inverse Compton scattering (ICS) of electrons (produced directly or in the prompt decay of $\mu, \tau$ leptons or in the hadronization of quarks produced in the annihilation of SODM) with the cosmic microwave background or starlight. | method 0.78 | 0.81 | 0.02 | asserted 0.90 |
| s3 | All these mechanisms yield significant contributions only for Higgs resonant exchange, i.e. for $M\approx M_{H}/2$, and the results depend on the Higgs scalar coupling to SODM, $g_{s}$. | result 0.96 | 0.82 | 0.08 | asserted 1.00 |
| s4 | The dominant mechanism at the GRE bump is the prompt photon production in the hadronization of $b$ quarks produced in $\bar{D}D\to \bar{b}b$, whereas the delayed photon emission from the ICS of electrons coming from the hadronization of $b$ quarks produced in the same reaction dominates at low energies ($\omega < 0.3~ GeV$) and prompt photons from $c$ and $\tau$, as well as from internal bremsstrahlung, yield competitive contributions at the end point of the spectrum ($\omega \ge 30 ~GeV$). | result 0.92 | 0.93 | 0.16 | asserted 1.00 |
| s5 | Taking into account all these contributions, our results for photons produced in the annihilation of SODM are in good agreement with the GRE data for $g_{s}\in [0.98, 1.01] \times 10^{-3}$ and $M\in [62.470,62.505]~GeV$. | result 1.00 | 0.96 | 0.84 | asserted 0.91 |
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The paper
Original abstract
In this work we study the possibility that the gamma ray excess (GRE) at the Milky Way galactic center come from the annihilation of dark matter with a $(1,0)\oplus(0,1)$ space-time structure (spin-one dark matter, SODM). We calculate the production of prompt photons from initial state radiation, internal bremsstrahlung, final state radiation including the emission from the decay products of the $\mu, \tau$ or hadronization of quarks. Next we study the delayed photon emission from the inverse Compton scattering (ICS) of electrons (produced directly or in the prompt decay of $\mu, \tau$ leptons or in the hadronization of quarks produced in the annihilation of SODM) with the cosmic microwave background or starlight. All these mechanisms yield significant contributions only for Higgs resonant exchange, i.e. for $M\approx M_{H}/2$, and the results depend on the Higgs scalar coupling to SODM, $g_{s}$. The dominant mechanism at the GRE bump is the prompt photon production in the hadronization of $b$ quarks produced in $\bar{D}D\to \bar{b}b$, whereas the delayed photon emission from the ICS of electrons coming from the hadronization of $b$ quarks produced in the same reaction dominates at low energies ($\omega < 0.3~ GeV$) and prompt photons from $c$ and $\tau$, as well as from internal bremsstrahlung, yield competitive contributions at the end point of the spectrum ($\omega \ge 30 ~GeV$). Taking into account all these contributions, our results for photons produced in the annihilation of SODM are in good agreement with the GRE data for $g_{s}\in [0.98, 1.01] \times 10^{-3}$ and $M\in [62.470,62.505]~GeV$.
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How the literature uses it
3 arXiv papers cite this in 3 sentences
What it cites · 56 sentences without a confident label
Uses the method or tool of 6 papers
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We calculate the complete prompt photon flux for $f=e,μ,τ,q,c,b$ using the tabulated spectrum defined as provided by DARKSUSY [ref] and PPC4DMID [ref] , including radiative corrections [ref] .
PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection · Final state radiation · 0.97
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We calculate the complete prompt photon flux for $f=e,μ,τ,q,c,b$ using the tabulated spectrum defined as provided by DARKSUSY [ref] and PPC4DMID [ref] , including radiative corrections [ref] .
On the Importance of Electroweak Corrections for Majorana Dark Matter Indirect Detection · Final state radiation · 0.97
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We calculate the complete prompt photon flux for $f=e,μ,τ,q,c,b$ using the tabulated spectrum defined as provided by DARKSUSY [ref] and PPC4DMID [ref] , including radiative corrections [ref] .
DarkSUSY: Computing Supersymmetric Dark Matter Properties Numerically · Final state radiation · 0.97
Uses data or values from 8 papers
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We take into account all these contributions to find the window for the SODM mass and couplings consistent with the GRE and uncertainties presented in [ref] .
The Fermi Galactic Center GeV Excess and Implications for Dark Matter · Spin-one dark matter annihilation into fermions and the GRE · 0.86
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There are stringent upper bounds on $⟨σv_r ⟩_γγ$ by FermiLAT [ref] and HESS [ref] collaborationsm, which for $M≈M_H/2$ are $⟨σv_r ⟩_γγ≤6.75 ×10^-29 cm^3/seg$.
Updated Search for Spectral Lines from Galactic Dark Matter Interactions with Pass 8 Data from the Fermi Large Area Telescope · Dark matter annihilation into two photons. · 0.93
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There are stringent upper bounds on $⟨σv_r ⟩_γγ$ by FermiLAT [ref] and HESS [ref] collaborationsm, which for $M≈M_H/2$ are $⟨σv_r ⟩_γγ≤6.75 ×10^-29 cm^3/seg$.
Search for $\gamma$-ray line signals from dark matter annihilations in the inner Galactic halo from ten years of observations with H.E.S.S · Dark matter annihilation into two photons. · 0.93
Compares with 5 papers
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In Fig. [ref] we show the upper bounds obtained by FermiLAT [ref] and our results for the window of SODM mass consistent with GRE data.
Updated Search for Spectral Lines from Galactic Dark Matter Interactions with Pass 8 Data from the Fermi Large Area Telescope · Dark matter annihilation into two photons. · 0.96
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In Fig. [ref] we plot the median expected limit and the region for $95%$ containment obtained in [ref] and our results for $1/2⟨σv_r ⟩_τ$ (the $1/2$ factor is required since the upper bounds are obtained for self-conjugated dark matter) .
Search for Gamma-Ray Emission from DES Dwarf Spheroidal Galaxy Candidates with Fermi-LAT Data · Annihilation into $μ^+μ^-$, $τ^+τ^-$ and $b̅ b$ · 0.91
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The photon energy flux from SODM annihilation into b-quark pairs, for each target, turns out to be smaller than the limits obtained using the bin-by-bin likelihood functions provided by FermiLAT-DES in the supplementary material of Ref. [ref] .
Searching for Dark Matter Annihilation in Recently Discovered Milky Way Satellites with Fermi-LAT · Annihilation into $μ^+μ^-$, $τ^+τ^-$ and $b̅ b$ · 0.96
Cites as background 21 papers
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During the past few years, it has been claimed by several groups that an excess over the expected gamma ray flux from known sources in the Milky Way galactic center exists in the FermiLAT data around $3 GeV$ [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] .
Dark Matter Annihilation in The Galactic Center As Seen by the Fermi Gamma Ray Space Telescope · GRE, prompt photons and muon inverse Compton scattering · 0.81
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During the past few years, it has been claimed by several groups that an excess over the expected gamma ray flux from known sources in the Milky Way galactic center exists in the FermiLAT data around $3 GeV$ [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] .
A comment on the emission from the Galactic Center as seen by the Fermi telescope · GRE, prompt photons and muon inverse Compton scattering · 0.81
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During the past few years, it has been claimed by several groups that an excess over the expected gamma ray flux from known sources in the Milky Way galactic center exists in the FermiLAT data around $3 GeV$ [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] [ref] .
On The Origin Of The Gamma Rays From The Galactic Center · GRE, prompt photons and muon inverse Compton scattering · 0.81
Discussion
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