论文标题
带有TEV伽马射线的银河光环中僻静的暗物质的当前和将来的限制
Present and Future constraints on Secluded Dark Matter in the Galactic Halo with TeV Gamma-ray Observatories
论文作者
论文摘要
暗物质遗物密度可以受到将暗物质场与标准模型颗粒联系起来的新介体的影响。当暗物质颗粒质量大于调解人时，介体的一对产生在运动学上是开放的。这种设置在文献中被称为僻静的暗物质。由于在几个模型建设努力中出现僻静的暗物质的动机，我们研究了南半球TEV伽马射线仪器的敏感性，即H.E.S.S.，CTA，SWGO和SWGO以僻静的暗物质在银河系中消灭了深色的暗物质。我们利用这些检测器的互补性方面，以在不同的歼灭通道的歼灭横截面上找到限制性界限。特别是，对于$ 2 $ 〜tev的暗物质粒子质量，H.E.S.S。能够约束$ \langleσv\ rangle \ geq 4 \ times 10^{ - 26} \，\，\，\，{\ rm cm}^3 \，{\ rm s}^{ - rm s}^{ - 1} $在95 \％的信心水平，$ 4Q $和$ 4q $ clunns，同时clys ne simessive unge n simessive the simestiment siveste to n simestive the simestive ty simestive the simessive。 \ geq 7 \ times 10^{ - 27} \，\，\，{\ rm cm}^3 \，{\ rm s}^{ - 1} $ and swgo $ \ langleσv\ rangleσv\ rangle \ geq 6 \ geq 6 \ times 10^{ - 27}} { - 27}}}}}}} $4τ$通道的s}^{ - 1} $，都远低于热遗物横截面。实际上，CTA和SWGO的组合将能够在整个质量范围内的暗物质颗粒范围低于100 GEV和100 TEV的$ 4Q $和$4τ$通道，以及100 GEV和100 GEV和$ \ sim $ 40 tev in $ 4B $通道中。
The dark matter relic density may be governed by the presence of new mediators that connect the dark matter field with the Standard Model particles. When the dark matter particle mass is larger than the mediator's, the pair production of mediators is kinematically open. This setup is known in the literature as secluded dark matter. Motivated by the appearance of secluded dark matter in several model building endeavours, we investigate the sensitivity of TeV gamma-ray instruments in the Southern Hemisphere namely, H.E.S.S., CTA, and SWGO to secluded dark matter annihilating in the Galactic Halo. We exploit the complementarity aspects of these detectors to find restrictive bounds on the annihilation cross-section for different annihilation channels. In particular, for a dark matter particle mass of $2$~TeV, H.E.S.S. is able to constraint $\langle σv \rangle \geq 4 \times 10^{-26}\,\, {\rm cm}^3\, {\rm s}^{-1}$ at 95\% confidence level for the $4q$ and $4τ$ channel, while CTA will be sensitive to $\langle σv \rangle \geq 7 \times 10^{-27}\,\, {\rm cm}^3\, {\rm s}^{-1}$ and SWGO $\langle σv \rangle \geq 6 \times 10^{-27}\,\, {\rm cm}^3\, {\rm s}^{-1}$ for the $4τ$ channel, both well below the thermal relic cross-section. In fact, the combination of CTA and SWGO will be able to probe cross-sections below the thermal relic value for dark matter particles in the whole mass range between 100 GeV and 100 TeV in the $4q$ and $4τ$ channels, and between 100 GeV and $\sim$40 TeV in the $4b$ channel.
