We present the first in depth dynamical analysis of the archetypal Wide-Angle Tailed (WAT) cluster Abell 562. We have combined Gemini observations with archival data from the literature to form a sample of 76 cluster members and derived a mean redshift of $0.1088 \pm 0.0004$ and a velocity dispersion of $919 \pm 116$ km s$^{-1}$. This relatively large velocity dispersion suggests either a very massive cluster ($M_{dyn} > 6.9 \times$ 10$^{14}$ $M_{sun}$) and/or a merger system. The merger model is supported by a non-Gaussian galaxy velocity distribution, an elongated spatial distribution of likely cluster members, and an elongated X-ray emitting gas. This scenario would generate the bulk flow motion of the intra-cluster medium that can exert enough ram pressure to bend the radio jets. Thus, our observations support the model in which a recent off-axis merger event produced the cluster wide conditions needed to shape the WAT in Abell 562.

中文翻译：

---

广角尾 (WAT) 星系团 A562 的动力学

我们首次对原型广角尾 (WAT) 星团 Abell 562 进行深度动态分析。我们将双子座观测与文献中的档案数据相结合，形成了 76 个星团成员的样本，并得出了平均红移 $0.1088 \pm 0.0004$ 和 $919 \pm 116$ km s$^{-1}$ 的速度色散。这种相对较大的速度离散表明一个非常大的星团（$M_{dyn} > 6.9 \times$ 10$^{14}$ $M_{sun}$）和/或合并系统。合并模型由非高斯星系速度分布、可能的星团成员的拉长空间分布和拉长的 X 射线发射气体支持。这种情况会产生簇内介质的大量流动运动，它可以施加足够的撞击压力来弯曲无线电射流。因此，