Cluster richness–mass calibration with cosmic microwave background lensing-猫眼课题宝

利用宇宙微波背景透镜进行团簇丰富度-质量校准

DOI：

10.1038/s41550-017-0259-1

发表时间：

2017

期刊：

Nature Astronomy

影响因子：

14.1

通讯作者：

中科院分区：

物理与天体物理1区

文献类型：

作者：

J. Geach;J. Peacock

与探测星团内高温介质的X射线5-7和Sunyaev-Zel‘dovich效应8探测方法相比，光度测量中通过星系密度过大来识别星系团是最古老的1，2也可以说是最经济和对质量敏感的探测方法3，4。然而，一个长期存在的问题是将光学“丰富度”测量映射到星系团的总质量3、9-12上。宇宙微波背景以14千兆秒的保角距离发射，对宇宙中所有中间的质量起到背光的作用，因此被引力透镜13-15所吸引。阿塔卡马宇宙学望远镜16、南极望远镜17-19和普朗克20卫星等实验现在已经探测到宇宙微波背景的引力透镜，并绘制了前景偏转结构的大面积地图。在这里，我们通过测量普朗克对大量光学选择的星系团位置的平均宇宙微波背景透镜，探测总质量为1014M⊙的结构对光子的偏转，在10%的水平上对星系团的光学丰度进行了定标。虽然主要是为了研究更大尺度的结构，但宇宙微波背景透镜场的普朗克估计可以用来恢复弧分尺度上堆积星系团的近乎无偏的透镜信号。这种方法提供了一种在大部分宇宙历史中对星系团总质量的干净测量，在很大程度上与重子物理无关。将星系团的光发射映射到其质量是具有挑战性的。大质量星系团对宇宙微波背景的透镜被用来在10%的水平上校准星系团的光学丰度与它们的总重子质量之比。

Identifying galaxy clusters through overdensities of galaxies in photometric surveys is the oldest1,2 and arguably the most economical and mass-sensitive detection method3,4, compared with X-ray5–7 and Sunyaev-Zel’dovich effect8 surveys that detect the hot intracluster medium. However, a perennial problem has been the mapping of optical ‘richness’ measurements onto total cluster mass3,9–12. Emitted at a conformal distance of 14 gigaparsecs, the cosmic microwave background acts as a backlight to all intervening mass in the Universe, and therefore has been gravitationally lensed13–15. Experiments such as the Atacama Cosmology Telescope16, South Pole Telescope17–19 and the Planck20 satellite have now detected gravitational lensing of the cosmic microwave background and produced large-area maps of the foreground deflecting structures. Here we present a calibration of cluster optical richness at the 10% level by measuring the average cosmic microwave background lensing measured by Planck towards the positions of large numbers of optically selected clusters, detecting the deflection of photons by structures of total mass of order 1014 M⊙. Although mainly aimed at the study of larger-scale structures, the Planck estimate of the cosmic microwave background lensing field can be used to recover a nearly unbiased lensing signal for stacked clusters on arcminute scales15,21. This approach offers a clean measure of total cluster masses over most of cosmic history, largely independent of baryon physics.Mapping the optical emission of a galaxy cluster to its mass is challenging. Lensing of the cosmic microwave background by massive clusters is used to calibrate the optical richness of clusters to their total baryonic mass at the ten per cent level.

A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA

DOI： 10.1088/0004-637x/756/2/142

发表时间： 2012-02

期刊：

The Astrophysical Journal

影响因子： --

作者：

A. V. Engelen;R. Keisler;O. Zahn;K. Aird;B. Benson;L. Bleem;J. Carlstrom;J. Carlstrom;C. Chang;C. Chang;Hsiao-mei Cho.;T. Crawford;A. Crites;T. Haan;M. Dobbs;J. Dudley;E. George;N. Halverson;G. Holder;W. Holzapfel;S. Hoover;Z. Hou;J. Hrubeš;M. Joy;L. Knox;Adrian T. Lee;Adrian T. Lee;E. Leitch;M. Lueker;D. Luong-Van;J. McMahon;J. Mehl;S. Meyer;M. Millea;J. Mohr;T. Montroy;T. Natoli;S. Padin;S. Padin;T. Plagge;C. Pryke;C. Reichardt;J. Ruhl;J. Sayre;K. Schaffer;K. Schaffer;L. Shaw;E. Shirokoff;H. Spieler;Z. Staniszewski;A. Stark;K. Story;K. Vanderlinde;J. Vieira;R. Williamson

通讯作者：

Cluster richness–mass calibration with cosmic microwave background lensing

利用宇宙微波背景透镜进行团簇丰富度-质量校准

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