论文标题
从z = 4.26射线星系4C 63.20扩展X射线排放
Extended X-ray emission from the z=4.26 radio galaxy 4C 63.20
论文作者
论文摘要
我们报道了4C 63.20的深色Chandra X射线望远镜成像观测值，这是Z> 3.5的少数已知射电星系之一。 X射线对应物被解析为核心，加上两个（组合）的核外来源，占总X射线通量的30％。它们的形态和取向与散布，类似叶的性质一致，尽管不能排除紧凑的热点。可以通过喷气模型复制4C 63.20的宽带光谱能量分布，其中大部分无线电通量可以归因于热点的同步器发射，其中（非核）X射线发射是通过compy Compton（IC）在cosmic microlofave（IC）中产生的，背景（CMB）内部的散布叶片。这种情况与更热的CMB中高度磁化叶的期望广泛一致，并支持IC/CMB可能会在高红移处淬灭极端的无线电裂片的观点。
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.
