A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA
A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA
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DOI：
10.1088/0004-637x/756/2/142
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发表时间：
2012-02
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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
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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
我们利用南极望远镜2008年和2009年的数据检测了引力透镜产生的宇宙微波背景（CMB）中的非高斯特征，并测量了投射引力势的功率谱。我们将透镜信号的测量幅度与基准ΛCDM宇宙学模型的预期幅度之比限制为0.86±0.16，在6.3σ处没有透镜不利。Wilkinson微波各向异性探测器（WMAP7）所允许的ΛCDM宇宙学模型的边缘化结果为Alens = 0.90±0.19，表明CMB透镜探测到的物质在红移范围0.5≤z≤5上的波动幅度与预测非常吻合。我们提出了几个一致性检查的结果。其中包括对CMB图中透镜特征的清晰检测，过滤后在傅里叶空间中没有重叠，以及与ΛCDM预期信号一致的“旋度”诊断。我们对由于噪声、前景和其他影响而导致的测量偏差进行了详细的研究，并确定与测量中的统计不确定性相比，这些贡献相对较小。我们将这种透镜测量结果与WMAP7的结果结合起来，与单独使用WMAP7的结果相比，改善了对宇宙学参数的约束：我们发现宇宙空间曲率的测量提高了3.9倍，Ωk =−0.0014±0.0172；在ΛCDM范围内，物质波动幅度提高10%，σ8 = 0.810±0.026；暗能量状态方程改进了5%，w =−1.04±0.40。与WMAP7与哈勃参数外部约束组合提供的w测量值相比，透镜数据的加入使w测量值提高了15%，得到w =−1.087±0.096。
We use South Pole Telescope data from 2008 and 2009 to detect the non-Gaussian signature in the cosmic microwave background (CMB) produced by gravitational lensing and to measure the power spectrum of the projected gravitational potential. We constrain the ratio of the measured amplitude of the lensing signal to that expected in a fiducial ΛCDM cosmological model to be 0.86 ± 0.16, with no lensing disfavored at 6.3σ. Marginalizing over ΛCDM cosmological models allowed by the Wilkinson Microwave Anisotropy Probe (WMAP7) results in a measurement of Alens = 0.90 ± 0.19, indicating that the amplitude of matter fluctuations over the redshift range 0.5 ≲ z ≲ 5 probed by CMB lensing is in good agreement with predictions. We present the results of several consistency checks. These include a clear detection of the lensing signature in CMB maps filtered to have no overlap in Fourier space, as well as a “curl” diagnostic that is consistent with the signal expected for ΛCDM. We perform a detailed study of bias in the measurement due to noise, foregrounds, and other effects and determine that these contributions are relatively small compared to the statistical uncertainty in the measurement. We combine this lensing measurement with results from WMAP7 to improve constraints on cosmological parameters when compared to those from WMAP7 alone: we find a factor of 3.9 improvement in the measurement of the spatial curvature of the universe, Ωk = −0.0014 ± 0.0172; a 10% improvement in the amplitude of matter fluctuations within ΛCDM, σ8 = 0.810 ± 0.026; and a 5% improvement in the dark energy equation of state, w = −1.04 ± 0.40. When compared with the measurement of w provided by the combination of WMAP7 and external constraints on the Hubble parameter, the addition of the lensing data improves the measurement of w by 15% to give w = −1.087 ± 0.096.