Abell 496中的多期喷发爆发：同步加速器老化与被暖气体纤维包裹的浮力X射线空腔
The Multi-Epoch Jet Outbursts in Abell 496: synchrotron ageing and buoyant X-ray cavities draped by warm gas filaments
AI总结：
本研究通过多波段观测揭示了Abell 496星系团中心射电星系与周围热气体的相互作用，发现三期喷流活动、两代X射线空腔及暖气体纤维对ICM冷却的刺激，并解释了未检测到射电迷你晕的现象。
摘要：
星系团Abell 496过去因大尺度上热气体的明显翻滚运动而被广泛研究，但中心射电星系与周围星系团大气之间的相互作用却鲜有探索。我们提出了一项针对Abell 496的专门射电、X射线和光学研究，旨在调查这一联系。我们使用Giant Metrewave Radio Telescope在150、330和617 MHz，Very Large Array在1.4和4.8 GHz，以及VLA Low Band Ionosphere and Transient Experiment在340 MHz获取的深度射电图像，角分辨率从0.5角秒到25角秒不等。此外，我们还使用了档案Chandra和Very Large Telescope MUSE观测数据。射电图像揭示了三个不同的喷流活动期：亚千秒差距尺度上正在进行的活动，具有倒转射电谱；较早的一期产生了约20千秒差距尺度的瓣，现在具有陡峭的谱指数（α= 2.0 ± 0.1）；最老的一期产生了约50 - 100千秒差距尺度的瓣，具有超陡谱（α= 2.7 ± 0.2）。档案Chandra X射线观测显示，较早和最老的活动期在星系团的热气体中挖掘出了两代空腔。最外层的X射线空腔具有明显的蘑菇头形状，可能是由其在星系团势阱中的浮力上升引起的。热气体的冷却在最内侧20千秒差距处仍在进行，在VLT-MUSE数据中可见Hα明亮的暖纤维。Hα纤维向蘑菇头空腔拉伸，可能刺激了其尾迹中的ICM冷却。最后，我们评论了在这个剧烈翻滚但低质量的星系团中未检测到射电迷你晕的情况。
英文摘要：
The galaxy cluster Abell 496 has been extensively studied in the past for the clear sloshing motion of the hot gas on large scales, but the interplay between the central radio galaxy and the surrounding cluster atmosphere is mostly unexplored. We present a dedicated radio, X-ray, and optical study of Abell 496 aimed at investigating this connection. We use deep radio images obtained with the Giant Metrewave Radio Telescope at 150, 330 and 617 MHz, Very Large Array at 1.4 and 4.8 GHz, and VLA Low Band Ionosphere and Transient Experiment at 340 MHz, with angular resolutions ranging from 0.''5 to 25''. Additionally, we use archival Chandra and Very Large Telescope MUSE observations. The radio images reveal three distinct periods of jet activity: an ongoing episode on sub-kpc scales with an inverted radio spectrum; an older episode that produced lobes on scales $\sim$20 kpc which now have a steep spectral index ($α= 2.0 \pm 0.1$); and an oldest episode that produced lobes on scales of $\sim$50 - 100 kpc with an ultra-steep spectrum ($α= 2.7 \pm 0.2$). Archival Chandra X-ray observations show that the older and oldest episodes have excavated two generations of cavities in the hot gas of the cluster. The outermost X-ray cavity has a clear mushroom-head shape, likely caused by its buoyant rise in the cluster's potential. Cooling of the hot gas is ongoing in the innermost 20 kpc, where H$α$-bright warm filaments are visible in VLT-MUSE data. The H$α$-filaments are stretched towards the mushroom-head cavity, which may have stimulated ICM cooling in its wake. We conclude by commenting on the non-detection of a radio mini-halo in this vigorously sloshing, but low-mass, galaxy cluster.
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