Abell 133中气体凝聚的测量
Measuring the gas clumping in Abell 133
摘要：
本文继续一系列，我们开发了一个非参数的方法来测量气体分布的不均匀性，从X射线观测的星系团。在这项工作中，我们将我们的方法应用到钱德拉X射线观测的Abell 133，并提出了确定的气体聚集因子的X射线团簇数据。我们发现Abell 133中的气体聚集因子随半径增加而增加，在$0.9\,R_{200}$处达到$\sim 2-3$。这与流体动力学模拟的预测和我们以前的确定是一致的。然后，我们观察到一个总体趋势，陡峭的径向轮廓的聚集校正的气体密度超过$0.3\, R_{200}$，与对数斜率的$\sim 2.6$在$0.9\,R_{200}$。与模拟相比，观测到的密度分布似乎更平坦，但与以前的观测结果一致。此外，我们观察到，测量的温度随着半径向A133的外围稳步下降，而熵随着半径单调增加，在外部体积中逐渐变平。相对于纯引力坍缩的理论预测，这里给出的结果指向中心区域的熵过剩，它延伸到大半径。这些结果表明，气体的不均匀性，应妥善处理时，解释X射线测量的信封星系团。最后，我们讨论了亮度分布如何保持记录的大尺度结构形成的情况下，提供了一个快照的“熔炉”的维里化区域。
英文摘要：
This paper continues a series in which we developed a non-parametric method to measure inhomogeneities in the gas distribution from X-ray observations of galaxy clusters. In this work, we apply our method to Chandra X-ray observations of Abell 133 and present the determination of the gas clumping factor from X-ray cluster data. We find that the gas clumping factor in Abell 133 increases with radius and reaches $\sim 2-3$ at $0.9\,R_{200}$. This is in good agreement with the predictions of hydrodynamical simulations and our previous determination. We then observe a general trend of steepening in the radial profiles of the clumping-corrected gas density beyond $0.3\, R_{200}$, with a logarithmic slope of $\sim 2.6$ at $0.9\,R_{200}$. The observed density profiles appear to be flatter compared to simulations, but in agreement with previous observational findings. In addition, we observe that the measured temperature decreases steadily with radius toward the outskirts of A133, while the entropy increases monotonically with radius, gently flattening in the outer volumes. With respect to theoretical predictions from pure gravitational collapse, the results presented here point to an entropy excess in the central regions, which extends out to large radii. These results suggest that gas inhomogeneities should be treated properly when interpreting X-ray measurements in the envelope of galaxy clusters. We finally discuss how the brightness distribution keeps a record of the large-scale structures formation scenario, providing a snapshot of the 'melting pot' in the virialization region.
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