发表机构
H.H. Wills Physics Laboratory, University of Bristol; National Centre for Radio Astrophysics, Pune（布里斯托大学H.H.威尔斯物理实验室; 浦那国家射电天文中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文利用钱德拉两期观测数据，首次对PKS 0637-752内喷流建立逆康普顿散射模型，并报告后退喷流射电瓣的X射线探测。
AI 中文摘要
我们利用两期存档的钱德拉（Chandra）观测数据（1999年和2017年），展示了类星体PKS 0637-752喷流的X射线表面亮度图。我们首次提出了从核心延伸3.4至7角秒的微弱内喷流模型，将其X射线发射解释为同步辐射相对论电子对宇宙微波背景光子的逆康普顿散射。内喷流与喷流明亮的外部区域形成对比，后者由多个离散的结节主导，费米（Fermi）伽马射线通量的上限排除了这些结节的逆康普顿机制。这是针对该内喷流发表的首个详细逆康普顿模型。我们考察了三种具有物理动机的情景，其区别在于电子分布的高能截断，这些情景能够解释观测到的射电、毫米/亚毫米和X射线发射，同时与光学和伽马射线上限保持一致。我们还首次报告了来自后退喷流末端射电瓣的X射线辐射。
英文摘要
We present the X-ray surface brightness maps of the jet from the quasar PKS 0637-752, using two epochs of archival Chandra observations (1999 and 2017). We present, for the first time, a model of the faint inner jet extending from 3.4 to 7 arcsec from the core, interpreting its X-ray emission as inverse Compton scattering of cosmic microwave background photons by the synchrotron-emitting relativistic electrons. The inner jet contrasts with the bright outer part of the jet, dominated by several discrete knots for which upper limits to the Fermi gamma-ray flux rule out the inverse Compton mechanism. It is the first detailed inverse Compton model published for this inner jet. We examine three physically motivated scenarios, distinguished by the high-energy cutoff of the electron distribution, that can account for the observed radio, millimeter/submillimeter, and X-ray emission while remaining consistent with optical and gamma-ray upper limits. We also report for the first time X-rays from the radio lobe at the end of the receding jet.
CommentsAccepted in ApJ. 21 pages, 10 figures
