We report on the X-ray emission from the radio jet of 3C 17 from Chandra observations and compare the X-ray emission with radio maps from the VLA archive and with the optical-IR archival images from the Hubble Space Telescope. X-ray detections of two knots in the 3C 17 jet are found and both of these features have optical counterparts. We derive the spectral energy distribution for the knots in the jet and give source parameters required for the various X-ray emission models, finding that both IC/CMB and synchrotron are viable to explain the high energy emission. A curious optical feature (with no radio or X-ray counterparts) possibly associated with the 3C 17 jet is described. We also discuss the use of curved jets for the problem of identifying inverse Compton X-ray emission via scattering on CMB photons.
Jet-Structure Imprint on the Curvature Tail of Gamma-Ray Burst Prompt Emission
Nanjing University（南京大学）；Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（现代天文与天体物理教育部重点实验室（南京大学））；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Center for Astronomical Mega-Science, Chinese Academy of Sciences（中国科学院天文大科学研究中心）；University of Bath（巴斯大学）；Institute for Astrophysics, School of Physics, Zhengzhou University（郑州大学物理学院天体物理研究所）；Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（高能物理研究所粒子天体物理教育部重点实验室）；University of Chinese Academy of Sciences（中国科学院大学）
伽马射线暴的曲率效应一直是人们关注的焦点。在准直的相对论伽玛射线暴喷流中，相对于观测者离轴的光子到达的时间比轴上的光子晚，并且预计光谱也会更软。在这项工作中，我们调用了一个相对简单的运动学两壳碰撞模型的均匀喷流剖面，并比较其预测的伽玛射线暴辐射数据的观测已归因于曲率效应，如峰值通量-峰值频率关系，即，伽玛暴脉冲衰减相的$ν$ F $_ν$通量与谱峰E $_{pk}$和谱滞后之间的关系。此外，我们探讨了脉冲宽度与能量的行为。我们提出的情况下，单脉冲费米伽玛暴110920，作为一个测试的预测模型对观测。
Spectropolarimetric detection of baryonic mass loading in a transient relativistic jet: application to the black hole X-ray binary Swift J1727.8$-$1613
Observational Properties of Thermal Emission from Relativistic Jets Embedded in AGN Disks
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Department of Astronomy, School of Physical Sciences, University of Science and Technology of China（中国科学技术大学物理学院天文学系）
