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 Multi-wavelength emissions from dark matter annihilation processes in galaxy clusters using cosmological simulations

2017 ◽  
Author(s):  
Remudin Reshid Mekuria ◽  
Sergio Colafrancesco ◽  
Andreas Faltenbacher ◽  
Paolo Marchegiani
Keyword(s):  
Dark Matter ◽  
Galaxy Clusters ◽  
Dark Matter Annihilation ◽  
Cosmological Simulations ◽  
Multi Wavelength

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 Gamma rays and neutrinos from dark matter annihilation in galaxy clusters

2010 ◽  
Vol 82 (2) ◽  
Author(s):  
Qiang Yuan ◽  
Peng-Fei Yin ◽  
Xiao-Jun Bi ◽  
Xin-Min Zhang ◽  
Shou-Hua Zhu
Keyword(s):  
Dark Matter ◽  
Galaxy Clusters ◽  
Gamma Rays ◽  
Dark Matter Annihilation

scholarly journals Bounds on dark matter annihilation cross-sections from inert doublet model in the context of 21-cm cosmology of dark ages

2021 ◽  
pp. 2150163
Author(s):  
Rupa Basu ◽  
Madhurima Pandey ◽  
Debasish Majumdar ◽  
Shibaji Banerjee
Keyword(s):  
Dark Matter ◽  
Cross Sections ◽  
Mass Range ◽  
Mass Region ◽  
High Mass ◽  
Dark Matter Annihilation ◽  
Dark Ages ◽  
Doublet Model ◽  
Inert Doublet Model ◽  
Text Signal

We study the fluctuations in the brightness temperature of 21-cm signal [Formula: see text] at the dark ages ([Formula: see text]) with a dark matter (DM) candidate in Inert Doublet Model (IDM). We then explore the effects of different fractions of IDM DM on [Formula: see text] signal. The IDM DM masses are chosen in few tens of GeV region as well as in the high mass region beyond 500 GeV. It has been observed that the [Formula: see text] signal is more sensitive in the DM mass range of 70–80 GeV. A lower bound on annihilation cross-section for this DM is also obtained by analyzing the [Formula: see text] signal. This is found to lie within the range [Formula: see text] cm3/s for the IDM DM mass range 10 GeV[Formula: see text] GeV.

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