从银河系中心重WIMP湮灭中二次光子发射的精细模型
A refined model of secondary photon emission from heavy WIMP annihilations in the Galactic Centre
AI总结：
本文提出了一种更精确的模型，用于研究银河系中心重WIMP湮灭产生的二次光子发射，通过考虑空间依赖性因素来提高检测重WIMPs的可能性。
摘要：
重弱相互作用大质量粒子（WIMPs）仍然是一个 prominent 但约束较少的暗物质（DM）候选者，银河系中心（GC）是通过伽马射线信号进行间接探测的首选目标。在扩展我们先前的工作，强调湮灭产生的电子的二次逆康普顿（IC）发射的重要性基础上，我们扩展分析范围到更广泛的WIMP质量，并引入更现实的GC环境空间依赖性建模框架。这种方法纳入了三维DM分布、空间变化的辐射和磁场、以及电子传输机制如银河风和扩散。我们评估了这些环境因素对所产生二次发射的空间和谱特性的影响。我们的结果展示了纳入这种发射的稳健性和必要性，并突显了其在通过观测内银河系检测重WIMPs方面的促进作用。我们提供由此产生的数据产品给社区，以支持未来的分析和观测研究。
英文摘要：
Heavy Weakly Interacting Massive Particles (WIMPs) remain a prominent yet less constrained dark matter (DM) candidate, with the Galactic Centre (GC) serving as a prime target for indirect detection via gamma-ray signals. Extending our previous work that highlighted the significance of secondary inverse Compton (IC) emission from annihilation-produced electrons, we expand the analysis to a broader range of WIMP masses and introduce a more realistic spatially-dependent modelling framework for the GC environment. This approach incorporates complexities such as the three-dimensional DM distribution, spatially varying radiation and magnetic fields, and electron transport mechanisms like Galactic winds and diffusion. We assess the impact of these environmental factors on both the spatial and spectral characteristics of the resulting secondary emissions. Our results demonstrate the robustness and necessity of incorporating this emission, and highlight its role in enhancing the prospects for detecting heavy WIMPs through observations of the inner Galaxy. We provide the resulting data products to the community to support future analyses and observational studies.
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