Search for gamma-ray spectral lines with the DArk Matter Particle Explorer

DAMPE (DArk Matter Particle Explorer) is a space mission project promoted by the Chinese Academy of Sciences (CAS), in collaboration with Universities and Institutes from China, Italy and Switzerland. The detector is collecting data in a stable sun-synchronous orbit lasting 95 minutes at an altitude of about 500 km. It has been launched in December 17th, 2015, from the Jiuquan Satellite Launch Center, in the Gobi Desert. The main goals of the mission are: indirect search for Dark Matter, looking for signatures in the electron and photon spectra with energies up to 10 TeV; analysis of the flux and composition of primary Cosmic Rays with energies up to hundreds of TeV; high energy gamma-ray astronomy. Preliminary results about the Helium flux and Cosmic Ray composition will be presented and discussed.

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Gamma-ray lines may reveal the CP nature of the dark matter particle

Journal of Cosmology and Astroparticle Physics ◽

10.1088/1475-7516/2019/01/047 ◽

2019 ◽

Vol 2019 (01) ◽

pp. 047-047 ◽

Cited By ~ 1

Author(s):

Farinaldo S. Queiroz ◽

Carlos E. Yaguna

Keyword(s):

Dark Matter ◽

Gamma Ray ◽

Dark Matter Particle

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Galactic Center Excess by Higgs Portal Dark Matter

International Journal of Modern Physics Conference Series ◽

10.1142/s2010194516601988 ◽

2016 ◽

Vol 43 ◽

pp. 1660198

Author(s):

Arindam Das ◽

Nobuchika Okada ◽

Osamu Seto

Keyword(s):

Dark Matter ◽

Gamma Ray ◽

Galactic Center ◽

Dark Matter Particle ◽

Higgs Doublet ◽

Parameter Region ◽

Dark Matter Search ◽

Real Scalar ◽

Dark Matter Relic Density ◽

Higgs Portal

A [Formula: see text] parity odd real scalar is a good candidate for dark matter in the present Universe. We consider models contain two Higgs doublet fields and one real scalar dark matter particle with mass in the range of [Formula: see text] GeV and annihilating into a [Formula: see text] pair, or with about [Formula: see text] GeV mass and annihilating into tau lepton pair. Those annihilation modes suitably explain the observed excess of the gamma-ray flux from the Galactic Center. We identify the parameter region of the model that can fit the gamma-ray excess and satisfy phenomenological constraints, such as the observed dark matter relic density and the null results of direct dark matter search experiments. Most of the parameter region is found to be within the search reach of various future experiments.

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Implications of dark matter cascade decay from DAMPE, HESS, Fermi-LAT and AMS02 data

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2924 ◽

2019 ◽

Cited By ~ 2

Author(s):

Yu Gao ◽

Yin-Zhe Ma

Keyword(s):

Dark Matter ◽

Gamma Ray ◽

Decay Channel ◽

Dark Matter Particle ◽

Cosmic Ray ◽

High Energy ◽

Data Sets ◽

Spectral Difference ◽

Cascade Decay ◽

Scale Down

Abstract Recent high-energy cosmic e± measurement from the DArk Matter Particle Explorer (DAMPE) satellite confirms the deviation of total cosmic ray electron spectrum above 700-900 GeV from a simple power law. In this paper we demonstrate that the cascade decay of dark matter can account for DAMPE’s TeV e+e− spectrum. We select the least constraint DM decay channel into four muons as the benchmark scenario, and perform an analysis with propagation variance in both DM signal and the Milky Way’s electron background. The best-fit of the model is obtained for joint DAMPE, Fermi-LAT, H.E.S.S. high energy electron data sets, and with an $\mathcal {O}(10^{26})$ second decay lifetime, which is consistent with existing gamma ray and cosmic microwave background limits. We compare the spectral difference between the cascade decay of typical final-state channels. The least constrained 4μ channels give good fits to the electron spectrum’s TeV scale down-turn, yet their low energy spectrum has tension with sub-TeV positron data from AMS02. We also consider a three-step cascade decay into eight muons, and also a gamma-ray constrained 4μ, 4b mixed channel, to demonstrate that a further softened cascade decay signal would be required for the agreement with all the data sets.

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Have scientists succeeded in detecting dark matter particle?

Editage Insights ◽

10.34193/ei-r-6603 ◽

2019 ◽

Author(s):

Editage Insights

Keyword(s):

Dark Matter ◽

Dark Matter Particle

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Detecting Cold Dark Matter Candidates

Symposium - International Astronomical Union ◽

10.1017/s0074180900150703 ◽

1987 ◽

Vol 117 ◽

pp. 490-490

Author(s):

A. K. Drukier ◽

K. Freese ◽

D. N. Spergel

Keyword(s):

Dark Matter ◽

Cold Dark Matter ◽

Galactic Halo ◽

Dark Matter Particle ◽

Low Energy ◽

The Sun ◽

Background Rate ◽

System Noise ◽

Weakly Interacting ◽

Massive Neutrinos

We consider the use of superheated superconducting colloids as detectors of weakly interacting galactic halo candidate particles (e.g. photinos, massive neutrinos, and scalar neutrinos). These low temperature detectors are sensitive to the deposition of a few hundreds of eV's. The recoil of a dark matter particle off of a superheated superconducting grain in the detector causes the grain to make a transition to the normal state. Their low energy threshold makes this class of detectors ideal for detecting massive weakly interacting halo particles.We discuss realistic models for the detector and for the galactic halo. We show that the expected count rate (≈103 count/day for scalar and massive neutrinos) exceeds the expected background by several orders of magnitude. For photinos, we expect ≈1 count/day, more than 100 times the predicted background rate. We find that if the detector temperature is maintained at 50 mK and the system noise is reduced below 5 × 10−4 flux quanta, particles with mass as low as 2 GeV can be detected. We show that the earth's motion around the Sun can produce a significant annual modulation in the signal.

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Spin-one dark matter and gamma ray signals from the galactic center

Journal of High Energy Physics ◽

10.1007/jhep08(2020)106 ◽

2020 ◽

Vol 2020 (8) ◽

Author(s):

H. Hernández-Arellano ◽

M. Napsuciale ◽

S. Rodríguez

Keyword(s):

Dark Matter ◽

Cross Section ◽

Gamma Ray ◽

Galactic Center ◽

Photon Emission ◽

Scalar Coupling ◽

Initial State ◽

Internal Bremsstrahlung ◽

Resonance Effects ◽

State Radiation

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) ⊕ (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 μ, τ 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 μ, τ 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 ≈ MH /2, and the results depend on the Higgs scalar coupling to SODM, gs. The dominant mechanism at the GRE bump is the prompt photon production in the hadronization of b quarks produced in $$ \overline{D}D\to \overline{b}b $$ D ¯ D → 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 (ω < 0.3 GeV ) and prompt photons from c and τ , as well as from internal bremsstrahlung, yield competitive contributions at the end point of the spectrum (ω ≥ 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 gs ∈ [0.98, 1.01] × 10−3 and M ∈ [62.470, 62.505] GeV . We study the consistency of the corresponding results for the dark matter relic density, the spin-independent dark matter-nucleon cross-section σp and the cross section for the annihilation of dark matter into $$ \overline{b}b $$ b ¯ b , τ+τ−, μ+μ− and γγ, taking into account the Higgs resonance effects, finding consistent results in all cases.

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