We report on deep Chandra X-ray Telescope imaging observations of 4C 63.20, one of the few known radio galaxies at z>3.5. The X-ray counterpart is resolved into a core plus two off-nuclear sources that (combined) account for close to 30% of the total X-ray flux. Their morphology and orientation are consistent with a diffuse, lobe-like nature, albeit compact hotspots cannot be ruled out. The broadband spectral energy distribution of 4C 63.20 can be reproduced with a jet model where the majority of the radio flux can be ascribed to synchrotron emission from the hotspots, whereas the (non-nuclear) X-ray emission is produced via Inverse Compton (IC) off of Cosmic Microwave Background (CMB) photons within the extended lobes. This scenario is broadly consistent with the expectation from highly magnetized lobes in a hotter CMB, and supports the view that IC/CMB may quench less extreme radio lobes at high redshifts.
A Chandra Study of the Radio Galaxy NGC 326: Wings, Outburst History, and AGN Feedback
NGC 326是最突出的X或Z形射电星系（XRG/ZRG）之一，并一直是几项研究的主题，试图通过流体运动或喷流轴的重新定向来解释其形态。我们研究了一个100 ks的档案钱德拉曝光，并发现与射电星系相关的几个功能：高温前，可能表明一个冲击，高温结周围的无线电发射的边缘，和一个腔与东翼的射电星系。根据射电数据对这些特征的合理解释使我们能够重建活动星系核爆发的历史。这次活跃的爆发很可能曾经是一个强大的射电源，但后来已经衰减，间接证据表明，重新定向是产生翅膀的手段。由于射电星系与ICM之间存在明显的相互作用，并且主动叶和翼之间存在很大的间隔，我们得出结论，XRG是通过测量与主动和被动加热机制相关的加热率来研究星系群中AGN反馈的极好来源。
A non cool-core 4.6-keV cluster around the bright nearby radio galaxy PKS B1416-493
我们提出了新的X射线（钱德拉）和无线电（ATCA）观测z=0.09射电星系PKS B1416-493，相当于南部的3CRR样本的成员。我们发现源嵌入在一个以前未被识别的明亮kT=4.6千电子伏非冷核心集群。在z=0.1的范围内发现如此高温度和亮度的新星系团是罕见的。根据其中间FRI/II形态选择射电源进行观测。我们确定了一个与东北瓣一致的腔，以及与西南瓣相关的过量计数，我们将其解释为逆康普顿X射线发射。喷流功率为5.3 x 10^44 erg/s，当用射电源密度加权时，支持了这样的观点，即中等形态和射电源的射电源可能主导了局部宇宙中的射电星系加热。
The radio source in Abell 980: A Detached-Double-Double Radio Galaxy?
UM-DAE Centre for Excellence in Basic Sciences, University of Mumbai（孟买大学基础科学卓越中心）；Department of Physics, Savitribai Phule Pune University（萨维特里巴伊·普勒浦那大学物理系）；INAF-Padova Astronomical Observatory（帕多瓦天文台）
