从星团内介质性质的多波长映射揭示$z = 1.2$最大质量MaDCoWS星团的合并动力学
Unveiling the merger dynamics of the most massive MaDCoWS cluster at $z = 1.2$ from a multi-wavelength mapping of its intracluster medium properties
摘要：
高红移星系团团内介质（ICM）性质的表征是理解星系团大尺度结构形成过程的基础。我们提出了一个非常巨大的集群MOO J1142 $+$ 1527在红移$z = 1.2$发现的大规模和遥远的集群的智慧巡天（MaDCoWS）的一部分，多波长分析的结果。该分析基于高角分辨率$Chandra$ X射线和NIKA 2 Sunyaev-Zel'dovich（SZ）数据。虽然X射线数据只有大约1700计数，我们能够确定ICM热力学径向轮廓，即温度，熵，和流体静力学质量。由于结合了高分辨率的X射线和SZ数据，这些数据在这个红移和$0.7R_{500}$之间以前所未有的精度获得。通过比较$Spitzer$的红外星系分布图和由$Chandra$和NIKA 2数据综合分析得到的ICM的形态特征，我们得出结论：该星系团是一个正在进行的合并。我们测量了以大尺度X射线质心为中心的四个角扇区中星团的流体静力学质量分布。这使我们能够估计一个系统的不确定性的集群总质量的特点所观察到的偏离球对称性和核心动力学的质量分布的影响。我们进一步结合X射线和SZ数据在像素级，以获得沿视线平均的温度和熵分布的地图。在X射线峰值处有一个相对低熵的核，在其南侧和西侧有高温区。考虑到合并动力学，预计SZ峰位置处ICM温度的增加。（节略）
英文摘要：
The characterization of the Intra-Cluster Medium (ICM) properties of high-redshift galaxy clusters is fundamental to our understanding of large-scale structure formation processes. We present the results of a multi-wavelength analysis of the very massive cluster MOO J1142$+$1527 at a redshift $z = 1.2$ discovered as part of the Massive and Distant Clusters of WISE Survey (MaDCoWS). This analysis is based on high angular resolution $Chandra$ X-ray and NIKA2 Sunyaev-Zel'dovich (SZ) data. Although the X-ray data have only about 1700 counts, we are able to determine the ICM thermodynamic radial profiles, namely temperature, entropy, and hydrostatic mass. These have been obtained with unprecedented precision at this redshift and up to $0.7R_{500}$, thanks to the combination of high-resolution X-ray and SZ data. The comparison between the galaxy distribution mapped in infrared by $Spitzer$ and the morphological properties of the ICM derived from the combined analysis of the $Chandra$ and NIKA2 data leads us to the conclusion that the cluster is an on-going merger. We measure the hydrostatic mass profile of the cluster in four angular sectors centered on the large-scale X-ray centroid. This allows us to estimate a systematic uncertainty on the cluster total mass that characterizes both the impact of the observed deviations from spherical symmetry and of the core dynamics on the mass profile. We further combine the X-ray and SZ data at the pixel level to obtain maps of the temperature and entropy distributions averaged along the line of sight. We find a relatively low entropy core at the position of the X-ray peak and high temperature regions located on its south and west sides. The increase in ICM temperature at the location of the SZ peak is expected given the merger dynamics. (abridged)
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