切伦科夫望远镜阵列观测英仙座星系团的 $\gamma$ 射线前景
高能天体物理现象
2024-10-25 v1 宇宙学与河外天体物理
高能物理 - 唯象学
摘要
星系团预期是暗物质（DM）的储库，也是沿星系团形成历史累积的宇宙线质子（CRp）的储存室。因此，它们是搜寻伽马射线能量下 DM 湮灭与衰变信号的优良目标，并由于星系团介质中的强子相互作用而被预言为大规模伽马射线辐射源。我们估算了切伦科夫望远镜阵列（CTA）探测英仙座星系团弥漫伽马射线辐射的灵敏度。我们对 DM 与 CRp 成分的预期信号进行了细致的空间与能谱建模，并分别计算了各成分预期的 CTA 灵敏度，同时讨论了英仙座的观测策略。在无非弥漫信号（未探测到）的情况下，对于遵循热气体空间分布且 CRp 谱指数 的 CRp 空间分布，CTA 应将半径 内的 CRp 与热能之比约束到约 。在英仙座射电迷你晕纯强子起源的乐观假设下，并取决于所假定的磁场轮廓，CTA 应将 测量到约 的精度，并将 CRp 空间分布以 10% 精度测定。关于 DM，CTA 应将当前来自星系团观测的地面伽马射线 DM 限制（对速度平均湮灭截面）提升最高达 倍，具体取决于 DM 晕子结构的建模。在 DM 粒子衰变情形下，CTA 将探索参数空间的新区域，对质量高于 1 TeV 的 DM 达到 s 的模型。这些约束将对星系团尺度的 CRp 加速与输运物理以及 TeV DM 粒子模型（尤其在衰变情景下）提供前所未有的灵敏度。
引用
@article{arxiv.2309.03712,
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journal= {arXiv preprint arXiv:2309.03712},
year = {2024}
}
备注
93 pages (including author list, appendix and references), 143 figures. Submitted to JCAP