Fitting dark matter mass with the radio continuum spectral data of the Ophiuchus cluster

Abstract

Recent gamma-ray and anti-proton analyses suggest that dark matter with mass m = 48 − 67 GeV annihilating via bb channel can explain the Galactic center GeV gamma-ray excess and the anti-proton excess as measured by AMS-02 simultaneously. In this article, by differentiating the contributions of dark matter annihilation and normal diffuse cosmic rays, we show that dark matter with mass m = 40 −50 GeV annihilating via bb channel with the thermal relic annihilation cross section can best explain the radio continuum spectrum of the central radio halo of the Ophiuchus cluster. This mass range, annihilation cross section, and the annihilation channel is completely consistent with the dark matter interpretations of the GeV gamma-ray excess and the anti-proton excess.

Constraining the spin-independent elastic scattering cross section of dark matter using the Moon as a detection target and the background neutrino data

“…tion to m χ ≈ 48 − 67 GeV as this range of annihilating dark matter mass can simultaneously explain the gammaray excess and anti-proton excess in our Galaxy [23][24][25]. This range can also explain some radio continuum data of galaxy clusters [26,27]. Therefore, our tighter constraints on the range m χ ≈ 48 − 56 GeV can provide some important complementary information of the particle dark matter.…”

Radio Constraints of Dark Matter: A Review and Some Future Perspectives

“…Besides the NFW profile, some other profiles may also be used for specific galaxies, such as the Burkert profile or the pseudo-isothermal profile [41]. For galaxy clusters, the hydrostatic density profile would be used as well [37,58]. The hydrostatic density profile depends on the thermal properties of the hot gas, which can be obtained easily from X-ray observations [58].…”

“…Therefore, fewer uncertainties would be involved compared with using the galactic radio data. Moreover, the radio contribution of the hot gas is insignificant (less than 1%) [37]. Hence, the major radio emissions in a galaxy cluster originate from two components only: dark matter annihilation and the background cosmic-ray contribution.…”

“…Recently, some studies have started to model the background cosmic-ray contributions [37][38][39]. If we could eliminate the background cosmic-ray contributions from the total radio emission, we could get much tighter constraints for annihilating dark matter.…”

“…Later, radio signals from other nearby galaxies such as the M31 [27][28][29], M33 [30,31], NGC 1569 [32], and NGC 2976 [33] galaxies were also investigated in constraining dark matter. Besides galactic radio signals, radio signals from galaxy clusters have been investigated [34][35][36][37][38][39]. Some other related studies such as the radio excess of extragalactic sources (e.g., ARCADEexcess) [40] have also been discussed in constraining dark matter.…”