AI 中文总结
该研究分析CHEX-MATE样本中116个星系团的X射线表面亮度不连续性，识别出66个特征（含32个新发现），并初步分类为8个疑似激波和34个冷锋，同时探讨了XMM数据分辨率限制带来的挑战。
AI 中文摘要
我们分析了CHEX-MATE样本中116个星系团的星系团内介质（ICM）中X射线表面亮度（SB）不连续性的存在，例如激波和冷锋。这些特征源于吸积相关过程，包括子团块合并到主星系团晕以及冷气体在较高熵环境中的晃动。我们通过检查SB残差（从观测中减去星系团模型获得）以及X射线图像上的梯度变化，在XMM CHEX-MATE图中识别这些结构。我们通过与文献中已描述的不连续性进行广泛分析和比较来验证我们的方法。我们的分析揭示了48个天体（约41%）中的66个不连续性，其中32个是新探测到的。我们发现，与扰动系统相比，弛豫系统中的不连续性往往更靠近核心、更弱，并且与全局X射线形态的排列程度更低。利用基于小波的温度图，我们提供了这些不连续性的初步分类，提出存在8个疑似激波和34个冷锋。此外，约48%具有扩展射电发射的系统显示出ICM不连续性的证据；相反，约88%探测到不连续性的天体具有相关的弥散射电发射。这项工作还探讨了使用XMM数据（其特点是空间分辨率相对较低）检测和分析此类特征的局限性，强调了仪器约束带来的挑战和潜在偏差。
英文摘要
We analyze the presence of X-ray surface brightness (SB) discontinuities, such as shocks and cold fronts, in the intracluster medium (ICM) of the 116 galaxy clusters from the CHEX-MATE sample. These features arise from accretion-related processes, including the merging of subclumps onto the main cluster halo and the sloshing of cold gas in a higher-entropy environment. We identify these structures in the XMM CHEX-MATE maps by examining both the SB residuals, obtained by subtracting a cluster model from the observations, and the gradient variations across X-ray images. We validate our method with an extensive analysis and comparison of the discontinuities described already in the literature. Our analysis reveals 66 discontinuities, 32 of which are newly detected, in 48 objects ($\sim$41%). We find that discontinuities in relaxed systems tend to be closer to the core, weaker, and less aligned with the global X-ray morphology compared to those in disturbed systems. Using wavelet-based temperature maps, we provide a preliminary classification of these discontinuities, proposing the occurrence of 8 putative shocks and 34 cold fronts. Furthermore, about 48% of the systems with extended radio emission show evidence of ICM discontinuities; conversely, $\sim$88% of the objects with detected discontinuities have an associated diffuse radio emission. This work also explores the limitations of using XMM data, characterized by relatively low spatial resolution, for detecting and analyzing such features, highlighting the challenges and potential biases introduced by instrumental constraints.
Comments12 pages, 8 figures. Accepted for publication in Astronomy & Astrophysics on 31 August 2026. Appendices A-I are available on Zenodo at https://doi.org/10.5281/zenodo.22715797
