什么是Cool-Core Cluster？X射线限流HIFLUGCS团簇样品的详细分析
What is a Cool-Core Cluster? A Detailed Analysis of the Cores of the X-ray Flux-Limited HIFLUGCS Cluster Sample
摘要：
我们使用最大的完整样本的64个星系团（最高X射线通量星系团样本）与现有的高质量的X射线数据从钱德拉，并应用16冷核心诊断，其中一些新的。我们还将最亮星系团的光学性质与X射线性质进行了关联。为了区分冷核和非冷核团簇，我们发现中心冷却时间t_cool是具有高质量数据的低红移团簇的最佳参数，而尖度是高红移团簇的最佳参数。在我们的样本中，72%的团簇具有冷核（t_cool < 7.7 h_{71} ^{-1/2} Gyr），44%具有强冷核（t_cool <1.0 h_{71} ^{-1/2} Gyr）。我们第一次定量地表明，在经典和光谱质量沉积速率的差异不能解释最近形成的冷芯，表明需要一个加热机制来解释冷却流问题。[摘要]
英文摘要：
We use the largest complete sample of 64 galaxy clusters (HIghest X-ray FLUx Galaxy Cluster Sample) with available high-quality X-ray data from Chandra, and apply 16 cool-core diagnostics to them, some of them new. We also correlate optical properties of brightest cluster galaxies (BCGs) with X-ray properties. To segregate cool core and non-cool-core clusters, we find that central cooling time, t_cool, is the best parameter for low redshift clusters with high quality data, and that cuspiness is the best parameter for high redshift clusters. 72% of clusters in our sample have a cool core (t_cool < 7.7 h_{71}^{-1/2} Gyr) and 44% have strong cool cores (t_cool <1.0 h_{71}^{-1/2} Gyr). For the first time we show quantitatively that the discrepancy in classical and spectroscopic mass deposition rates can not be explained with a recent formation of the cool cores, demonstrating the need for a heating mechanism to explain the cooling flow problem. [Abridged]
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