论文标题
与银河系核心大小的暗物质自我交流的限制
Constraints on dark matter self-interaction from galactic core size
论文作者
论文摘要
颗粒暗物质的自相互作用可能有助于热热化银河晕和驱动核心形成的中心区域。核心半径预期对暗物质（DM）的自我交互强度敏感。在本文中，我们研究了从孤立光环中核心半径的分布来限制暗物质自我相互作用的可行性。我们仅在$ 10^{10} $ - $ 10^{15} m _ {\ odot} $的质量范围内对球形对称的孤立的银河系光环进行系统的DM模拟，并结合了等于同型DM自我互动的影响。将模拟配置文件与观察数据进行比较，我们为自我交叉截面提供了保守的上限，$σ /m <$ 9.8 $ $ \ \ \ \ \ rm cm^2 /\ rm gm $ $ 95 \％$ $ puterity $ prustice Level。我们报告了派生界限对用于分析的银河密度分布模型的显着依赖性。
Self-interaction of particulate dark matter may help thermalising the central region of the galactic halo and driving core formation. The core radius is expectedly sensitive to the self-interaction strength of dark matter (DM). In this paper we study the feasibility of constraining dark matter self-interaction from the distribution of the core radius in isolated haloes. We perform systematic DM only $N$-body simulations of spherically symmetric isolated galactic haloes in the mass range of $10^{10} $-$10^{15}M_{\odot}$, incorporating the impact of isotropic DM self-interaction. Comparing the simulated profiles with the observational data, we provide a conservative upper limit on the self-interaction cross-section, $ σ/m < $ $ 9.8 $ $\ \rm cm^2 /\rm gm $ at $ 95 \% $ confidence level. We report significant dependence of the derived bounds on the galactic density distribution models assumed for the analysis.
