The Dark Matter Annihilation Signal from Dwarf Galaxies and Subhalos
The Dark Matter Annihilation Signal from Dwarf Galaxies and Subhalos
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DOI：
10.1155/2010/162083
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发表时间：
2009-06
影响因子：
1.4
通讯作者：
M. Kuhlen
中科院分区：
文献类型：
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作者：
M. Kuhlen
暗物质湮灭具有直接探测银河系晕的巨大潜力，这是冷暗物质等级结构形成范式的关键预测之一。在这里，我们回顾了银河系暗晕中心暗物质湮灭产生的γ射线信号。𝛾我们认为这两个已知的银河系矮卫星星系和黑暗的团块没有恒星的组成部分作为潜在的来源。利用通过Lactea II数值模拟，我们估计通量18银河系矮椭球与公布的中心密度。最有希望的来源是Segue 1，其次是Ursa Major II，Ursa Minor，Draco和Carina。我们表明，如果任何已知的银河系卫星可以被检测到，那么至少有十倍以上的subhalos应该是可见的，其中很大一部分是黑暗的团块。
Dark Matter annihilation holds great potential for directly probing the clumpiness of the Galactic halo that is one of the key predictions of the Cold Dark Matter paradigm of hierarchical structure formation. Here we review the 𝛾-ray signal arising from dark matter annihilation in the centers of Galactic subhalos. We consider both known Galactic dwarf satellite galaxies and dark clumps without a stellar component as potential sources. Utilizing the Via Lactea II numerical simulation, we estimate fluxes for 18 Galactic dwarf spheroidals with published central densities. The most promising source is Segue 1, followed by Ursa Major II, Ursa Minor, Draco, and Carina. We show that if any of the known Galactic satellites can be detected, then at least ten times more subhalos should be visible, with a significant fraction of them being dark clumps.