每一个具有强大无线电AGN的BCG都有一个X射线冷却核心：冷却核心和非冷却核心的二分法是否过于简单？
Every BCG with a strong radio AGN has an X-ray cool core: is the cool core - noncool core dichotomy too simple?
摘要：
X射线冷核中的射电活动星系核反馈被认为是重子结构演化的重要组成部分。然而，人们早就知道强射电活动星系核也存在于“非冷核”星系团中，这就提出了一个问题，即射电反馈是否总是需要一个X射线冷核。在这项工作中，我们提出了一个系统的分析BCGs和强射电活动星系核在152组和集群从钱德拉档案。所有69个射电活动星系核在1.4 GHz时亮度超过2 × 10^23 W Hz^-1的BCG都被发现具有X射线冷核。BCG冷芯可分为两类，大冷芯（LCC）类和电晕类。在z>0.1时很容易被忽视的小日冕，可以在大的冷核形成之前很久就在群体和集群中引发强烈的加热事件。日冕引发的强烈射电爆发可能会摧毁胚胎大冷核，从而提供另一种机制来防止大冷核的形成。然而，目前还不清楚日冕是否与无线电反馈周期脱钩，因为它们必须在很大程度上不受强烈的无线电爆发的影响。我们的样本研究还表明，没有一个发光的冷核心，而托管一个强大的无线电活动星系核，这是没有观察到的集群组。这表明，无线电加热对低质量系统的影响比集群更大。作为日冕类的例子，我们还详细分析了与强射电活动星系核（A3627中的ESO 137-006）和已知最暗日冕之一（半人马座星系团中的NGC 4709）相关的BCG日冕。我们的研究结果表明，传统的冷芯/非冷芯二分法是过于简单。一个更好的替代方法是冷核分布函数，其中包含X射线光度或气体质量。
英文摘要：
Radio AGN feedback in X-ray cool cores has been proposed as a crucial ingredient in the evolution of baryonic structures. However, it has long been known that strong radio AGN also exist in "noncool core" clusters, which brings up the question whether an X-ray cool core is always required for radio feedback. In this work, we present a systematic analysis of BCGs and strong radio AGN in 152 groups and clusters from the Chandra archive. All 69 BCGs with radio AGN more luminous than 2x10^23 W Hz^-1 at 1.4 GHz are found to have X-ray cool cores. The BCG cool cores can be divided into two classes, the large-cool-core (LCC) class and the corona class. Small coronae, easily overlooked at z>0.1, can trigger strong heating episodes in groups and clusters, long before large cool cores are formed. Strong radio outbursts triggered by coronae may destroy embryonic large cool cores and thus provide another mechanism to prevent formation of large cool cores. However, it is unclear whether coronae are decoupled from the radio feedback cycles as they have to be largely immune to strong radio outbursts. Our sample study also shows the absence of groups with a luminous cool core while hosting a strong radio AGN, which is not observed in clusters. This points to a greater impact of radio heating on low-mass systems than clusters. As examples of the corona class, we also present detailed analyses of a BCG corona associated with a strong radio AGN (ESO 137-006 in A3627) and one of the faintest coronae known (NGC 4709 in the Centaurus cluster). Our results suggest that the traditional cool core / noncool core dichotomy is too simple. A better alternative is the cool core distribution function, with the enclosed X-ray luminosity or gas mass.
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