高音谱号射电凤凰及其古老的非热丝状结构
The Treble Clef radio phoenix and its old nonthermal filaments
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- INAF - IRA（意大利国家天体物理研究所）
- Center for Astrophysics | Harvard & Smithsonian（哈佛-史密松天体物理中心）
- Space Research Institute (IKI)（空间研究所）
- Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）
- Rudolf Peierls Centre for Theoretical Physics, Department of Physics, University of Oxford（牛津大学理论物理鲁道夫·派尔斯中心）
- Hamburger Sternwarte（汉堡天文台）
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中文总结 AI 辅助
研究低银纬处奇特丝状射电源，结合X射线观测与多频率数据，表征宿主星系团性质并分析射电源，结论是其为射电凤凰，形态受合并中气体运动影响，是低频后续观测理想目标。
中文摘要 AI 辅助
通过检查低频阵列两米天空调查（LoTSS）的数据，我们在低银纬（$b \approx 0.5 °$）处发现了一个奇特的明亮丝状射电源。该源在先前的射电观测中也被探测到，最初被认为是一颗脉冲星，直到格林等人（2004年）提出它位于银盘后面一个被严重遮挡的星系团中。在本文中，我们首次利用钱德拉和SRG/eROSITA进行的X射线观测来表征宿主星系团的主要性质（红移、质量、温度、X射线光度和动力学状态）。此外，通过将新的uGMRT后续数据与低频阵列低频段全天调查（LoLSS）的观测结果相结合，我们对丝状射电源（VLSS J0318.9+5755，因其形态在此处昵称为“高音谱号”）进行了多频率、空间分辨的光谱分析。我们得出结论，这个源是一个属于在回避区内一个大质量合并星系团的射电凤凰。我们推测其复杂的形态是由正在进行的合并过程中星系团介质中产生的气体运动塑造的，这些运动也可能是在星系团中心初步观测到的候选射电晕产生的原因。由于其高度丝状的形态、在$\lesssim$1 GHz的亮度以及极其陡峭的光谱，在400到650 MHz之间达到$\alpha > 4$的值，这个源是使用LOFAR2.0进行高分辨率、甚低频后续观测的理想目标。
英文摘要
By inspecting data from the LOFAR Two-meter Sky Survey (LoTSS), we noticed a peculiar bright and filamentary radio source at low-galactic latitude ($b \approx 0.5 °$). This source, detected also in previous radio observations, was originally believed to be a pulsar, but was later suggested to be located in a heavily obscured galaxy cluster behind the Galactic plane. In this paper, we characterize for the first time the main properties of the host cluster (redshift, mass, temperature, X-ray luminosity, and dynamical status) by using X-ray observations performed with Chandra and SRG/eROSITA. In addition, by combining new uGMRT follow-up data with observations from the e LOFAR LBA Sky Survey (LoLSS), we perform a multifrequency, spatially resolved spectral analysis of the filamentary radio source (VLSS J0318.9+5755, nicknamed here the "Treble Clef" due to its morphology). We conclude that this source is a radio phoenix belonging to a massive, merging galaxy cluster in the Zone of Avoidance. We speculate that its complex morphology is shaped by gas motions generated in the intracluster medium during the ongoing merger, which are also likely responsible for the generation of the candidate radio halo tentatively observed in the cluster center. Owing to its highly filamentary morphology, brightness at $\lesssim$1 GHz, and extremely steep spectrum, reaching values of $α> 4$ between 400 and 650 MHz, this source represents an ideal target for high-resolution, very-low-frequency follow-up observations with LOFAR2.0.
