A joint ALMA–Bolocam–Planck SZ study of the pressure distribution in RX J1347.5−1145
A joint ALMA–Bolocam–Planck SZ study of the pressure distribution in RX J1347.5−1145
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ALMA-Bolocam-Planck SZ 联合研究 RX J1347.5−1145 中的压力分布
DOI：
10.1093/mnras/stz1550
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发表时间：
2018
影响因子：
4.8
通讯作者：
T. Mroczkowski
中科院分区：
文献类型：
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作者：
L. Di Mascolo;E. Churazov;T. Mroczkowski
我们报告了对来自星系团 RX J1347.5−1145 的 Sunyaev-Zeldovich (SZ) 效应的单碟和干涉观测的联合分析。我们开发了一种使用本机成像和可见性数据的参数拟合程序，并使用 ALMA、Bolocam 和 Planck 可用于此物体的丰富数据集对其进行了测试。 RX J1347.5−1145 是一个非常炽热且明亮的星团，显示出合并的迹象。之前的 X 射线驱动的 SZ 研究强调了 X 射线峰值东南部存在过量的 SZ 信号，这通常被解释为强烈的冲击引起的压力扰动。当我们的模型以 X 射线峰值为中心时，证实了这一点。然而，两个几乎同样明亮的巨大椭圆星系的存在使得星系团中心的选择变得模糊，并且在星系团结构的建模中具有相当大的自由度。例如，我们已经证明，SZ 信号可以通过单个光滑椭球体广义纳瓦罗-弗伦克-怀特轮廓来很好地描述，其中最拟合的质心位于两个最亮的星系团之间。这导致来自东南下部结构的多余 SZ 信号显着减弱。此外，X射线中看到的最突出的特征可以解释为主要是等压结构，从而减轻了对高超音速的需求，尽管与移动亚晕相关的超压区域仍然存在于我们的模型中。
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 ∼100 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.
哈勃太空望远镜结合强弱透镜分析碰撞样本：质量和放大率模型以及系统不确定性
DOI：
10.1088/0004-637x/801/1/44
发表时间：
2015
期刊：
The Astrophysical Journal
影响因子：
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作者：
A. Zitrin;A. Fabris;J. Merten;P. Melchior;M. Meneghetti;A. Koekemoer;D. Coe;M. Maturi;M. Bartelmann;M. Postman;K. Umetsu;G. Seidel;I. Sendra;T. Broadhurst;I. Balestra;A. Biviano;C. Grillo;A. Mercurio;M. Nonino;P. Rosati;L. Bradley
通讯作者：
L. Bradley
TolTEC毫米波相机的光学设计
DOI：
10.1117/12.2314130
发表时间：
2018
期刊：
SPIE Astronomical Telescopes and Instrumentation 2018
影响因子：
--
作者：
Bryan, Sean A.;Austermann, Jason E.;Mauskopf, Philip;Novak, Giles;Simon, Sara M.;Wilson, Grant W.;McMahon, Jeff;Ferrusca, Daniel;Montana, Alfredo;Sanchez-Arguelles, David
通讯作者：
Sanchez-Arguelles, David
影响因子：
4.8
作者：
Churazov, E.;Arevalo, P.;Zhuravleva, I.
通讯作者：
Zhuravleva, I.