切伦科夫望远镜阵列观测站对矮椭球星系中暗物质观测的前景
高能天体物理现象
2025-11-26 v3 星系天体物理
天体物理仪器与方法
摘要
围绕银河系运行的矮椭球星系（dSphs）被广泛认为是靠速度弥散对抗自引力支撑的系统，并且由于缺乏天体物理 γ 射线背景，它们成为在 GeV 至 TeV γ 射线波段搜寻间接暗物质（DM）信号的主要目标。我们给出了即将建成的切伦科夫望远镜阵列观测站（CTAO）对这些目标中湮灭或衰变暗物质信号的灵敏度预测。我们从当前已知天体目录中进行了候选体的原始筛选，包括经典和超暗矮椭球星系。对于每个候选体，我们使用最全面的测光和光谱数据，在一致的分析框架内推导出预期的暗物质含量。这种方法使我们能够推导出用于间接暗物质搜寻的新天体物理因子轮廓，并与文献中的结果进行了比较。从最初的 64 个矮椭球星系样本中，我们确定了八个有前景的目标——北天的 Draco I、Coma Berenices、Ursa Major II、Ursa Minor 和 Willman 1，以及南天的 Reticulum II、Sculptor 和 Sagittarius II——对于这些目标，不同的暗物质密度模型给出了一致的预期，从而产生了稳健的预测。CTAO 预计将在约 10 TeV 以上提供最强的限制，对于组合限制，其速度平均湮灭截面可达约 5×10^{-25} cm^3 s^{-1}，衰变寿命可达约 10^{26} s。主要的不确定性源于暗物质含量的不精确测定，特别是对于超暗矮椭球星系。我们提出了观测策略，以优化对最佳候选体的深度曝光或多样化的目标选择。
引用
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Zhang and V. I. Zhdanov and M. Živec and J. Zuriaga-Puig},
journal= {arXiv preprint arXiv:2508.19120},
year = {2025}
}
备注
40 pages, 19 figures, 10 tables, accepted for publication on MNRAS