A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND GRAVITATIONAL LENSING POTENTIAL FROM 100 SQUARE DEGREES OF SPTPOL DATA
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND GRAVITATIONAL LENSING POTENTIAL FROM 100 SQUARE DEGREES OF SPTPOL DATA
复制标题
根据 100 平方度的 SPTPOL 数据测量宇宙微波背景引力透镜势
DOI：
10.1088/0004-637x/810/1/50
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
O. Zahn
中科院分区：
文献类型：
--
作者：
K. Story;D. Hanson;P. Ade;K. Aird;J. Austermann;J. Beall;A. Bender;A. Bender;B. Benson;B. Benson;L. Bleem;L. Bleem;J. Carlstrom;C. Chang;C. Chang;H. Chiang;H.;R. Citron;T. Crawford;A. Crites;A. Crites;T. Haan;M. Dobbs;M. Dobbs;W. Everett;J. Gallicchio;Jiansong Gao;E. George;A. Gilbert;N. Halverson;N. Harrington;J. Henning;J. Henning;G. Hilton;G. Holder;W. Holzapfel;S. Hoover;Z. Hou;J. Hrubeš;N. Huang;J. Hubmayr;K. Irwin;R. Keisler;L. Knox;Adrian T. Lee;Adrian T. Lee;E. Leitch;Dale Li;Dale Li;C. Liang;D. Luong;J. McMahon;J. Mehl;J. Mehl;S. Meyer;L. Mocanu;T. Montroy;T. Natoli;J. Nibarger;V. Novosad;S. Padin;S. Padin;C. Pryke;C. Reichardt;C. Reichardt;J. Ruhl;B. Saliwanchik;J. Sayre;K. Schaffer;K. Schaffer;G. Smecher;A. Stark;C. Tucker;K. Vanderlinde;J. Vieira;Gensheng Wang;N. Whitehorn;V. Yefremenko;O. Zahn
我们利用 SPTpol（目前安装在南极望远镜上的偏振敏感接收器）前两个季节的观测数据，对宇宙微波背景 (CMB) 引力透镜势进行了测量。这项工作中使用的观测覆盖了 100 deg2 的天空，分辨率为 150 GHz 的弧分。使用二次估计器，我们根据 CMB 温度和偏振图的组合制作了 CMB 透镜效应图。我们将这些透镜势图组合起来形成最小方差（MV）图。对于100<L<250°>之间的角多极，透镜效应是用大于1的信噪比来测量的。这是迄今为止由 CMB 制作的最高信噪比质量图，并且与其他大型结构示踪剂的互相关性很强。我们计算每个估计量的透镜效应的功率谱，并报告 100 < L < 2000 ?> 之间的 MV 功率谱值作为我们的主要结果。我们将频谱与基准 ΛCDM 模型的比率限制为 AMV = 0.92 ± 0.14 (Stat.) ± 0.08 (Sys.)。仅限制极化数据，我们发现 APOL = 0.92 ± 0.24（统计）± 0.11（系统）。该测量结果拒绝了 5.9 &sgr 处无透镜效应的假设。 ?> 单独使用偏振数据，并且在 14 &sgr; ?> 使用温度和偏振数据。
We present a measurement of the cosmic microwave background (CMB) gravitational lensing potential using data from the first two seasons of observations with SPTpol, the polarization-sensitive receiver currently installed on the South Pole Telescope. The observations used in this work cover 100 deg2 of sky with arcminute resolution at 150 GHz. Using a quadratic estimator, we make maps of the CMB lensing potential from combinations of CMB temperature and polarization maps. We combine these lensing potential maps to form a minimum-variance (MV) map. The lensing potential is measured with a signal-to-noise ratio of greater than one for angular multipoles between 100 < L < 250 ?> . This is the highest signal-to-noise mass map made from the CMB to date and will be powerful in cross-correlation with other tracers of large-scale structure. We calculate the power spectrum of the lensing potential for each estimator, and we report the value of the MV power spectrum between 100 < L < 2000 ?> as our primary result. We constrain the ratio of the spectrum to a fiducial ΛCDM model to be AMV = 0.92 ± 0.14 (Stat.) ± 0.08 (Sys.). Restricting ourselves to polarized data only, we find APOL = 0.92 ± 0.24 (Stat.) ± 0.11 (Sys.). This measurement rejects the hypothesis of no lensing at 5.9 &sgr; ?> using polarization data alone, and at 14 &sgr; ?> using both temperature and polarization 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：
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
DOI：
10.1088/0004-637x/722/2/1180
发表时间：
2010-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
通讯作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
影响因子：
8.6
作者：
Ade, P. A. R.;Aikin, R. W.;Yoon, K. W.
通讯作者：
Yoon, K. W.