這項研究計算了星系團中暗物質湮滅的無線電通量密度。該研究假設這些星團中的暗物質由卡魯扎-克萊因粒子 (KKDM) 組成。 KKDM 指的是在宇宙額外維度中運動的粒子，是冷暗物質候選者之一。 KKDM 的自湮滅會導致相對論性電子-正電子對，這會在具有高磁場的星系團中產生顯著的同步輻射射電輻射。為了對這些漫射無線電發射設置下限約束，我們分析了產生費米子對的通道中的通量密度，例如 e+e-、μ+μ- 和 τ+τ-。該研究發現，如果 KKDM 是這些星團中的主要暗物質，那麼富星團（例如 Abell 119 和 Abell 2029）可能會從 KKDM 湮滅中產生可檢測的漫射無線電發射。這項研究為了解星系團中 KKDM 的特性提供了寶貴的見解，並進一步了解了宇宙學和暗物質搜索的意義。;This study calculates the radio flux density from dark matter annihilations in galaxy clusters. The research assumes that the dark matter in these clusters is composed of Kaluza-Klein particles (KKDM). KKDM refers to particles moving in the universal extra dimensions and is one of the cold dark matter candidates. Self-annihilation of KKDM could result in relativistic electron-positron pairs, which can generate significant synchrotron radio emission in galaxy clusters with high magnetic fields. To set the lower limit constraints on these diffuse radio emissions, we analyzed the flux density in channels producing fermion pairs, such as e+e-, μ+μ-, and τ+τ-. The study found that a rich cluster, such as the Abell 119 and Abell 2029 might create possible detectable diffuse radio emission from KKDM annihilation if the KKDM is the main dark matter in these clusters. This research offers valuable insights into the properties of KKDM in galaxy clusters and provides further understanding of the implications of cosmology and dark matter searches.
