Here we present detailed analysis of the distinct X-ray emission features present within the Eastern radio lobe of the Pictor A galaxy, around the jet termination region, utilising the data obtained from the Chandra X-ray Observatory. Various emission features have been selected for the study based on their enhanced X-ray surface brightness, including five sources that appear point-like, as well as three extended regions, one characterised by a filamentary morphology. For those, we perform a basic spectral analysis within the 0.5-7keV range. We also investigate various correlations between the X-ray emission features and the non-thermal radio emission, utilising the high-resolution radio maps from the Very Large Array at GHz frequencies. The main novel findings following from our analysis, regard the newly recognized bright X-ray filament located upstream of the jet termination region, extending for at least thirty kiloparsec (projected), and inclined with respect to the jet axis. For this feature, we observe a clear anti-correlation between the X-ray surface brightness and the polarized radio intensity, as well as a decrease in the radio rotation measure with respect to the surroundings. We speculate on the nature of the filament, in particular addressing a possibility that it is related to the presence of a hot X-ray emitting thermal gas, only partly mixed with the non-thermal radio/X-ray emitting electrons within the lobe, combined with the reversals in the lobe's net magnetic field.
Discovery of gamma-ray emission from the Broad Line Radio Galaxy Pictor A
本文报道了基于费米大天区望远镜（LAT）三年的观测，发现宽线射电星系（BLRG）绘架座A的高能γ射线辐射，其显著性为~5.8σ（TS=33.4）。三年平均E>0.2 GeV的γ射线能谱可用幂律方程描述，光子指数为Γ，积分通量为$2.93 \pm 0.03$ ph cm $^{-2}$ s $^{-1}$。对观测到的γ射线通量进行时间调查，将通量分为一年长的间隔，发现第三年的通量比三年平均通量高50%。这一观察，再加上这一来源的事实，没有检测到在头两年的{费米-LAT观测，表明一年或更少的时间尺度上的变化。同步辐射自康普顿模拟的光谱能量分布的一个突出的热点在绘架座A的西部射电瓣进行。结果发现，γ射线发射起源于叶内的模型预测的X射线通量大于观测值。鉴于射电瓣热点中的X射线发射已经用目前的X射线探测器套件解决了，我们认为Pictor A的γ射线发射来自其喷流内部，这与其他γ射线大声BLRG一致。这一建议与γ射线通量在一年或更短的时间尺度上变化的证据一致。
The Western Jet of SS 433/W50: Hard X-ray Emission, Spectral Evolution, and Comparison to the Eastern Jet
University of Manitoba（曼尼托巴大学）；Chinese Academy of Sciences（中国科学院）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）；Columbia Astrophysics Laboratory（哥伦比亚天体物理实验室）；University of California San Diego（加州大学圣地亚哥分校）；Institute for Cosmic Ray Research, University of Tokyo（东京大学宇宙射线研究所）
利用 NuSTAR 和 XMM-Newton 观测，在 W50 西瓣检测到高达 30 keV 的硬非热 X 射线发射，源自“头部”区域，具有硬光子指数 1.55，并呈现远离 SS 433 的谱变陡，与东瓣对称，支持喷流驱动起源。
Investigation of the Microquasar SS 433 with VERITAS
DePauw University（迪保大学）；Temple University（天普大学）；University of Utah（犹他大学）；University College Dublin（都柏林大学学院）；University of California, Los Angeles（加州大学洛杉矶分校）；California Polytechnic State University（加州州立理工大学）；Washington University（华盛顿大学）；Santa Cruz Institute for Particle Physics（圣克鲁兹粒子物理研究所）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
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。
