The investigation of dark matter density profiles on the neutralino mass and cross-section annihilation (mχ−〈σv〉) constraint lines of selected galaxy clusters by considering their synchrotron emission

We investigated the indirect detection of neutralino dark matter using radio observation. By looking at the energy spectrum of relativistic positron–electron, this method may provide us with the upper limit of neutralino dark matter emission. Neutralino dark matter can emit synchrotron emissions due to the interaction of relativistic positron–electron spectrum energy with the intracluster magnetic field. The synchrotron emission of dark matter highly depends on the dark matter density at the centre of the cluster. By using the cold dark matter model, the density of dark matter can be obtained using Navarro–Frenk–White (NFW), Einasto, Diemer and Kravtsov 2014 (DK14) and Hernquist profiles. Using the observed radio halo emission as the maximum emission (from dark matter and other sources), we constrained the neutralino mass (mχ) and neutralino cross-section annihilation 〈σv〉 as mχ−〈σv〉 constraint lines. We investigated the effect of different profiles on the mχ−〈σv〉 constraint lines. We also used all the basic annihilation channels for better and stronger constraint lines. Our findings demonstrated the NFW profiles provided us with a good constraint line similarly with previous study. Our results also confirmed that the τ+τ− and tt̄ channels provide us with a stronger constraint at mχ = 100 GeV and 1000 GeV, respectively. Overall, our findings are consistent for the constraint lines of all the chosen galaxy clusters namely A119, A2199, A2142, A2744, A478 and A2029. •Important steps in reducing the uncertainty in estimating the density of dark matter particles.•Successfully investigated stronger annihilation channels for neutralino dark matter.•Deduced that the Hernquist and NFW profiles produced the best constraint lines.•Found that tau+ tau- provides a stronger constraint for neutralino masses of 100 GeV and 1000 GeV, respectively.