In this work, we study the potential of the Cherenkov Telescope Array (CTA) for the detection of Galactic dark matter (DM) subhalos. We focus on low-mass subhalos that do not host any baryonic content and therefore lack any multiwavelength counterpart. If the DM is made of weakly interacting massive particles (WIMPs), these dark subhalos may thus appear in the gamma-ray sky as unidentified sources. A detailed characterization of the instrumental response of CTA to dark subhalos is performed, for which we use the ctools analysis software and simulate CTA observations under different array configurations and pointing strategies, such as the scheduled extragalactic survey. This, together with information on the subhalo population as inferred from N-body cosmological simulations, allows us to predict the CTA detectability of dark subhalos, i.e., the expected number of subhalos in each of the considered observational scenarios. In the absence of detection, for each observation strategy we set competitive limits to the annihilation cross section as a function of the DM particle mass, that are at the level of $〈\sigma v〉\sim 4\times 10^{-24}$ ($7\times 10^{-25}$) ${\mathrm{cm}}^3{s}^{-1}$ for the $b\bar{b}$ (${\tau }^{+}{\tau }^{-}$) annihilation channel in the best case scenario. Interestingly, we find the latter to be reached with no dedicated observations, as we obtain the best limits by just accumulating exposure time from all scheduled CTA programs and pointings over the first 10 years of operation. This way CTA will offer the most constraining limits from subhalo searches in the intermediate range between $\sim 1-3\mathrm{TeV}$, complementing previous results with Fermi-LAT and HAWC at lower and higher energies, respectively.

在这项工作中，我们研究了切伦科夫望远镜阵列 (CTA) 探测银河暗物质 (DM) 亚晕的潜力。我们专注于不包含任何重子内容的低质量亚晕，因此缺乏任何多波长对应物。如果 DM 是由弱相互作用的大质量粒子 (WIMP) 组成的，那么这些黑暗的亚晕可能因此作为不明来源出现在伽马射线天空中。对 CTA 对暗亚晕的仪器响应进行了详细的表征，为此我们使用了ctools分析软件并模拟不同阵列配置和指向策略下的 CTA 观测，例如预定的河外调查。这与从 N 体宇宙学模拟推断的亚晕种群信息一起，使我们能够预测暗亚晕的 CTA 可探测性，即每个考虑的观测场景中亚晕的预期数量。在没有检测的情况下，对于每个观察策略，我们将湮灭截面的竞争限制设置为 DM 粒子质量的函数，其水平为$〈\sigma v〉～4\times 10^{-24}$ ($7\times 10^{-25}$) ${\mathrm{厘米}}^3{秒}^{-1}$ 为了 $乙\overline{乙}$ (${\tau }^{+}{\tau }^{-}$) 最佳情况下的湮灭通道。有趣的是，我们发现后者不需要专门的观察​​就可以达到，因为我们只是通过从所有计划的 CTA 程序和前 10 年运行的指示中累积曝光时间来获得最佳限制。通过这种方式，CTA 将在介于两者之间的中间范围内从 subhalo 搜索中提供最严格的限制。$～1-3\mathrm{伏特}$，分别在较低和较高能量下用Fermi -LAT 和 HAWC补充了先前的结果。