ALMA-Bolocam-Planck SZ对RX J1347中压力分布的联合研究。5 -1145
A joint ALMA-Bolocam-Planck SZ study of the pressure distribution in RX J1347.5-1145
摘要：
我们报告了对星系团RX J1347.5-1145的Sunyaev-Zeldovich（SZ）效应的单碟和干涉观测的联合分析。我们已经开发了一个参数拟合程序，使用本地成像和可见度数据，并使用丰富的数据集ALMA，Bolocam，普朗克可用于此对象进行测试。RX J1347.5-1145是一个非常热和明亮的星团，显示出合并的特征。以前的X射线驱动的SZ研究强调了存在一个多余的SZ信号东南的X射线峰，这通常被解释为一个强大的，冲击引起的压力扰动。我们的模型，当中心在X射线峰时，证实了这一点。然而，两个几乎同样明亮的巨大椭圆星系被$\sim100\;{\rm kpc}$分开，使得星系团中心的选择变得模糊不清，并允许在建模星系团的结构时有相当大的自由度。例如，我们已经表明，SZ信号可以很好地描述了一个单一的平滑椭圆广义Navarro-Frenk-White的配置文件，其中最适合的质心位于两个最明亮的星系团之间。这导致了一个相当弱的过剩SZ信号从东南部的子结构。此外，在X射线中看到的最突出的特征可以解释为主要的等压结构，减轻了对高超音速的需要，尽管与移动的subhaloes相关的过压区域仍然存在于我们的模型中。
英文摘要：
We report the joint analysis of single-dish and interferometric observations of the Sunyaev-Zeldovich (SZ) effect from the galaxy cluster RX J1347.5-1145. We have developed a parametric fitting procedure that uses native imaging and visibility data, and tested it using the rich data sets from ALMA, Bolocam, and Planck available for this object. RX J1347.5-1145 is a very hot and luminous cluster showing signatures of a merger. Previous X-ray-motivated SZ studies have highlighted the presence of an excess SZ signal south-east of the X-ray peak, which was generally interpreted as a strong, shock-induced pressure perturbation. Our model, when centred at the X-ray peak, confirms this. However, the presence of two almost equally bright giant elliptical galaxies separated by $\sim100\;{\rm kpc}$ makes the choice of the cluster centre ambiguous, and allows for considerable freedom in modelling the structure of the galaxy cluster. For instance, we have shown that the SZ signal can be well-described by a single smooth ellipsoidal generalized Navarro-Frenk-White profile, where the best-fitting centroid is located between the two brightest cluster galaxies. This leads to a considerably weaker excess SZ signal from the south-eastern substructure. Further, the most prominent features seen in the X-ray can be explained as predominantly isobaric structures, alleviating the need for highly supersonic velocities, although overpressurized regions associated with the moving subhaloes are still present in our model.
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