Non-thermal radio emission from dark matter annihilation processes in simulated Coma like galaxy clusters

2019 ◽  
Vol 15 (S356) ◽  
pp. 385-387
Author(s):  
Fitsum Woldegerima Beyene ◽  
Remudin Reshid Mekuria
Keyword(s):  
Dark Matter ◽  
Radio Emission ◽  
Galaxy Clusters ◽  
Small Deviation ◽  
Branching Ratio ◽  
Annihilation Process ◽  
Coma Cluster ◽  
Dark Matter Annihilation ◽  
Annihilation Channel ◽  
Radio Halo

AbstractTaking secondary particles produced from dark matter (DM) annihilation process to the origin of the extended diffuse radio emission observed in galaxy clusters, we studied both their morphology and radio spectral profile using simulated Coma like galaxy clusters. We have considered a neutralino annihilation channel dominated by $b\overline b $ species with a branching ratio of 1 and neutralino mass of 35 GeV with annihilation cross-section of 1×10-26 cm3 s-1. The radio emission maps produced for the two simulated galaxy clusters which are based on the MUsic SImulation of galaxy Clusters (MUSIC) dataset reveal the observed radio halo morphology showing radio emission both from the central regions of the cluster and substructures lying out off cluster centre. The flux density curve is in a good agreement for ν ≤ 2 GHz with the obsevational values for the Coma cluster of galaxies showing a small deviation at higher frequencies.

scholarly journals Effect of turbulent reacceleration on electrons produced by dark matter annihilation in the Coma cluster

2019 ◽  
Vol 488 (1) ◽  
pp. 1401-1406 ◽  
Author(s):  
P Marchegiani
Keyword(s):  
Dark Matter ◽  
Gamma Ray ◽  
Coma Cluster ◽  
Dark Matter Annihilation ◽  
Annihilation Channel ◽  
Radio Halo ◽  
Upper Limits ◽  
Astrophysical Objects ◽  
Conservative Values ◽  
Short Times

ABSTRACT In this paper, we study the effect of reacceleration provided by turbulences on electrons produced by dark matter (DM) annihilation in the Coma cluster. We use a simplified phenomenological model to describe the effect of the turbulences, and explore a limited subset of three possible DM models for neutralino particles with different mass and annihilation channel. We find that, for values of the annihilation cross-section of the order of the upper limits found with Fermi–LAT measurements in astrophysical objects, and for conservative values of the boosting factor due to DM substructures, the reacceleration due to turbulences can enhance the radio emission produced by DM-originated electrons up to the level of the observed flux of the radio halo in Coma, for moderate reacceleration intensity in relatively short times. Therefore, we conclude that, even if it is not possible to distinguish between the fits obtained in this paper because of the scattering present in the radio flux data, the electrons produced by DM annihilation can be possible seed electrons for the reacceleration, as well as secondary electrons of hadronic origin. A possible discriminant between these two classes of models is the flux produced in the gamma ray band, which in the case of DM-originated electrons should be more than two orders of magnitude smaller than the present Fermi–LAT upper limits, whereas in the hadronic case the expected gamma ray flux should be close to the value of present upper limits.

Multi-wavelength emission from dark matter annihilation processes in galaxy clusters and dark matter sub-halos

2019 ◽  
Vol 15 (S356) ◽  
pp. 390-392
Author(s):  
Remudin Reshid Mekuria
Keyword(s):  
Dark Matter ◽  
Radio Emission ◽  
Galaxy Clusters ◽  
High Mass ◽  
Stellar Content ◽  
Dark Matter Annihilation ◽  
Multi Wavelength ◽  
Crucial Information ◽  
Wavelength Emission ◽  
Statistical Studies

AbstractMulti-wavelength emission maps from dark matter (DM) annihilation processes in galaxy clusters are produced using Marenostrum-MultiDark SImulation of galaxy Clusters (MUSIC-2) high resolution cosmological simulations. Comparison made with observational radio emission flux data (spectral shape) and the spatial distribution from the simulated emission maps show that secondary particles from DM annihilation could describe the origin of energetic particles which are the sources of the diffuse radio emission observed in large number of galaxy clusters. DM sub-halos which are dominantly composed of DM, but with very little or no gas and stellar content, are ideal objects to study the nature and properties of DM. Therefore, statistical studies of a large number of them as well the emission maps of high mass-to-light ratio DM sub-halos will not only explain the observed diffused radio emission but also provide very crucial information about the nature and properties of DM particles.

scholarly journals NEUTRINO EMISSION FROM DARK MATTER ANNIHILATION/DECAY IN LIGHT OF COSMIC e± AND $\bar{p}$ DATA

2012 ◽  
Vol 27 (06) ◽  
pp. 1250024 ◽  
Author(s):  
JIE LIU ◽  
QIANG YUAN ◽  
XIAOJUN BI ◽  
HONG LI ◽  
XINMIN ZHANG
Keyword(s):  
Dark Matter ◽  
Branching Ratio ◽  
Cosmic Ray ◽  
Current Data ◽  
Neutrino Emission ◽  
Dark Matter Annihilation ◽  
Text Data ◽  
Self Consistent ◽  
Γ Rays ◽  
Global Fitting

A self-consistent global fitting method based on the Markov Chain Monte Carlo technique to study the dark matter (DM) property associated with the cosmic ray electron/positron excesses was developed in our previous work. In this work we further improve the previous study to include the hadronic branching ratio of DM annihilation/decay. The PAMELA [Formula: see text] data are employed to constrain the hadronic branching ratio. We find that the 95% (2σ) upper limits of the quark branching ratio allowed by the PAMELA [Formula: see text] data is ~0.032 for DM annihilation and ~0.044 for DM decay, respectively. This result shows that the DM coupling to pure leptons is indeed favored by the current data. Based on the global fitting results, we further study the neutrino emission from DM in the galactic center. Our predicted neutrino flux is some smaller than previous works since the constraint from γ-rays is involved. However, it is still capable to be detected by the forthcoming neutrino detector such as IceCube. The improved points of the present study compared with previous works include: (1) the DM parameters, both the particle physical ones and astrophysical ones, are derived in a global fitting way, (2) constraints from various species of data sets, including γ-rays and antiprotons are included, and (3) the expectation of neutrino emission is fully self-consistent.

scholarly journals Particle Reacceleration by Turbulence and Radio Constraints on Multimessenger High-energy Emission from the Coma Cluster

2021 ◽  
Vol 922 (2) ◽  
pp. 190
Author(s):  
Kosuke Nishiwaki ◽  
Katsuaki Asano ◽  
Kohta Murase
Keyword(s):  
Galaxy Clusters ◽  
Gamma Ray ◽  
Radial Profile ◽  
Planck Equation ◽  
High Energy ◽  
Coma Cluster ◽  
Radio Halo ◽  
Energy Emission ◽  
Neutrino Fluxes ◽  
High Energy Emission

Abstract Galaxy clusters are considered to be gigantic reservoirs of cosmic rays (CRs). Some of the clusters are found with extended radio emission, which provides evidence for the existence of magnetic fields and CR electrons in the intra-cluster medium. The mechanism of radio halo (RH) emission is still under debate, and it has been believed that turbulent reacceleration plays an important role. In this paper, we study the reacceleration of CR protons and electrons in detail by numerically solving the Fokker–Planck equation, and show how radio and gamma-ray observations can be used to constrain CR distributions and resulting high-energy emission for the Coma cluster. We take into account the radial diffusion of CRs and follow the time evolution of their one-dimensional distribution, by which we investigate the radial profile of the CR injection that is consistent with the observed RH surface brightness. We find that the required injection profile is nontrivial, depending on whether CR electrons have a primary or secondary origin. Although the secondary CR electron scenario predicts larger gamma-ray and neutrino fluxes, it is in tension with the observed RH spectrum for hard injection indexes, α < 2.45. This tension is relaxed if the turbulent diffusion of CRs is much less efficient than the fiducial model, or the reacceleration is more efficient for lower-energy CRs. In both the secondary and primary scenario, we find that galaxy clusters can make a sizable contribution to the all-sky neutrino intensity if the CR energy spectrum is nearly flat.

scholarly journals Lepton dark matter portal in the inert Zee model

2020 ◽  
Vol 35 (31) ◽  
pp. 2050190
Author(s):  
Alexandra Gaviria ◽  
Robinson Longas ◽  
Andrés Rivera
Keyword(s):  
Dark Matter ◽  
Parameter Space ◽  
Tree Level ◽  
Neutrino Masses ◽  
Dark Matter Annihilation ◽  
Annihilation Channel ◽  
Flavor Changing ◽  
Inert Doublet Model ◽  
Relic Abundance ◽  
The Impact

The inert Zee model is an extension of the Zee model for neutrino masses. This new model explains the dark matter relic abundance, generates a one-loop neutrino masses and forbids tree-level Higgs-mediated flavor changing neutral currents. Although the dark matter phenomenology of the model is similar to that of the inert doublet model, the presence of new vector-like fermions opens the lepton portal as a new dark matter annihilation channel. We study the impact of this new portal in the low-mass regime and show the parameter space allowed by direct and indirect searches of dark matter. Remarkably, the region for [Formula: see text] GeV is recovered for [Formula: see text]. We also show that future experiments like LZ and DARWIN could probe a large region of the parameter space of the model.

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