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18 April 2024

» arxiv » 1412.7521

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A Measurement of Gravitational Lensing of the Cosmic Microwave Background by Galaxy Clusters Using Data from the South Pole Telescope
E. J. Baxter ; R. Keisler ; S. Dodelson ; K. A. Aird ; S. W. Allen ; M. L. N. Ashby ; M. Bautz ; M. Bayliss ; B. A. Benson ; L. E. Bleem ; S. Bocquet ; M. Brodwin ; J. E. Carlstrom ; C. L. Chang ; I. Chiu ; H-M. Cho ; A. Clocchiatti ; T. M. Crawford ; A. T. Crites ; S. Desai ; J. P. Dietrich ; T. de Haan ; M. A. Dobbs ; R. J. Foley ; W. R. Forman ; E. M. George ; M. D. Gladders ; A. H. Gonzalez ; N. W. Halverson ; N. L. Harrington ; C. Hennig ; H. Hoekstra ; G. P. Holder ; W. L. Holzapfel ; Z. Hou ; J. D. Hrubes ; C. Jones ; L. Knox ; A. T. Lee ; E. M. Leitch ; J. Liu ; M. Lueker ; D. Luong-Van ; A. Mantz ; D. P. Marrone ; M. McDonald ; J. J. McMahon ; S. S. Meyer ; M. Millea ; L. M. Mocanu ; S. S. Murray ; S. Padin ; C. Pryke ; C. L. Reichardt ; A. Rest ; J. E. Ruhl ; B. R. Saliwanchik ; A. Saro ; J. T. Sayre ; K. K. Schaffer ; E. Shirokoff ; J. Song ; H. G. Spieler ; B. Stalder ; S. A. Stanford ; Z. Staniszewski ; A. A. Stark ; K. T. Story ; A. van Engelen ; K. Vanderlinde ; J. D. Vieira ; A. Vikhlinin ; R. Williamson ; O. Zahn ; A. Zenteno ;
Date:	23 Dec 2014
Abstract:	Clusters of galaxies are expected to gravitationally lens the cosmic microwave background (CMB) and thereby generate a distinct signal in the CMB on arcminute scales. Measurements of this effect can be used to constrain the masses of galaxy clusters using CMB data alone. Here we present a measurement of lensing of the CMB by galaxy clusters using data from the South Pole Telescope (SPT). We develop a maximum likelihood approach to extract the CMB cluster lensing signal and validate the method on mock data. We quantify the effects of several potential sources of systematic error and find that they generally act to reduce the best-fit cluster mass. The net magnitude of the systematic shift to lower cluster mass is approximately the size of our statistical error bar, and we do not attempt to correct for it. We apply the maximum likelihood technique to 513 clusters selected via their SZ signatures in SPT data, and rule out the null hypothesis of no lensing at 3.0$sigma$. The lensing-derived mass estimate for the full cluster sample is consistent with that inferred from the SZ flux: $M_{200, m{lens}} = 0.76^{+0.37}_{-0.36} M_{200, m{SZ}}$ (68% C.L., statistical error only).
Source:	arXiv, 1412.7521
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