标题： 暗物质-重子相互作用截面的星系团热力学约束 显示英文标题

标题： Constraints on the dark matter-baryon interaction cross section from galaxy cluster thermodynamics

摘要： 暗物质(DM)模型中，如果暗物质与重子之间的相互作用截面不为零，则意味着暗物质与重子之间存在能量传递。我们提出了一种新的方法，利用星系团的热力学特性来限制速度无关相互作用的暗物质-重子相互作用截面和暗物质粒子质量。如果这些星系团中的重子气体处于热力学平衡状态，并且暗物质使重子冷却，那么这种冷却速率受到星系团中其他机制的净加热速率的限制。我们使用了来自X射线探测星系团的元目录(MCXC)的REFLEX星系团，并采用了阿塔卡马宇宙学望远镜(ACT)的苏尼亚耶夫-泽尔多维奇(SZ)选定的星系团目录中的质量估计。这给出了速度无关相互作用下暗物质-质子相互作用截面的95%上限，分别为$\sigma_0\leq9.3\times10^{-28} \mathrm{~cm^2}$和$m_\chi = 10^{-4} - 10^{-1}$GeV。这些约束在这个质量范围内的最佳约束的一个数量级之内，并作为补充的独立约束。我们还将此模型应用于部分相互作用的暗物质情景，其中只有10%和1%的暗物质在相互作用。与其他方法不同，这个约束与该比例成线性关系。这给出了95%的上限$\sigma_0\leq1.1\times10^{-26} \mathrm{~cm^2}$和$\sigma_0\leq8.2\times10^{-26} \mathrm{~cm^2}$，这是该情景下目前最强的约束。本文作为一个概念验证。即将到来的SZ测量将提供星系团的温度剖面。将这些测量结果与更复杂的热力学模型相结合，可能会导致更稳健的约束。 显示英文摘要

摘要： Dark matter (DM) models with a non-zero DM-baryon interaction cross section imply energy transfer between DM and baryons. We present a new method of constraining the DM-baryon interaction cross section and DM particle mass for velocity-independent interactions using the thermodynamics of galaxy clusters. If the baryonic gas in these clusters is in thermodynamic equilibrium and DM cools baryons, this cooling rate is limited by the net heating rate of other mechanisms in the cluster. We use the REFLEX clusters from the Meta-Catalogue of X-ray detected Clusters of Galaxies (MCXC) with mass estimates from the Atacama Cosmology Telescope (ACT) catalog of Sunyaev-Zel'dovich (SZ) selected galaxy clusters. This yields 95% upper bounds on the DM-proton interaction cross section for velocity-independent interactions of $\sigma_0\leq9.3\times10^{-28} \mathrm{~cm^2}$ for DM masses, $m_\chi = 10^{-4} - 10^{-1}$ GeV. These constraints are within an order of magnitude of the best constraints derived in this mass range, and serve as a complementary, independent constraint. We also apply this model to the fractional interacting DM scenario, where only 10% and 1% of the DM is interacting. Unlike other methods, this constraint scales linearly with this fraction. This yields 95% upper bounds of $\sigma_0\leq1.1\times10^{-26} \mathrm{~cm^2}$ and $\sigma_0\leq8.2\times10^{-26} \mathrm{~cm^2}$, which are the strongest existing constraints for this scenario. This paper serves as a proof of concept. Upcoming SZ measurements will provide temperature profiles for galaxy clusters. Combining these measurements with more complex thermodynamic models could lead to more robust constraints.