SECOND SEASON QUIET OBSERVATIONS: MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRUM AT 95 GHz
SECOND SEASON QUIET OBSERVATIONS: MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRUM AT 95 GHz
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第二季安静观测：95 GHz 宇宙微波背景偏振功率谱的测量
DOI：
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发表时间：
2012
期刊：
影响因子：
--
通讯作者：
R. Williamson
中科院分区：
文献类型：
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作者：
Q. C. D. Araujo;C. Bischoff;A. Brizius;I. Buder;Y. Chinone;K. Cleary;R. N. Dumoulin;A. Kusaka;R. Monsalve;S. Naess;L. Newburgh;R. Reeves;I. Wehus;J. Zwart;L. Bronfman;R. Bustos;S. Church;C. Dickinson;H. Eriksen;T. Gaier;J. Gundersen;M. Hasegawa;M. Hazumi;K. Huffenberger;K. Ishidoshiro;M. Jones;P. Kangaslahti;D. Kapner;D. Kubik;C. Lawrence;M. Limon;J. McMahon;A. Miller;M. Nagai;H. Nguyen;G. Nixon;T. Pearson;L. Piccirillo;Simon J. E. Radford;A. Readhead;J. Richards;D. Samtleben;M. Seiffert;M. Shepherd;K. Smith;S. Staggs;O. Tajima;K. Thompson;K. Vanderlinde;R. Williamson
Q/U成像实验（QUIET）观测到了43和95 GHz的宇宙微波背景辐射（CMB）。43 GHz的结果已经发表在以前的论文中，在这里，我们报告的测量CMB偏振功率谱使用95 GHz的数据。该数据集包括由84个偏振相干接收器组成的阵列记录的5337小时的观测，阵列的总灵敏度为87 μ K。观测到了四个低前景场，覆盖了总共1000 deg2，有效角分辨率为12. ′ 8，允许对原始引力波的约束和跨越三个声学峰的E模式的高信噪比测量。使用两个独立的分析流水线进行数据减少，一个基于伪C_∞（PCL）互相关方法，另一个基于最大似然（ML）方法。在检查任何非零功率谱之前，修改所有数据选择标准和过滤器，直到满足预定义的一组零测试。两条管道的计算结果吻合较好。我们在λ = 25和975之间描述了EE、EB和BB功率谱，发现EE功率谱与Λ CDM一致，而BB功率谱与零一致。基于这些测量，我们将张量与标量之比限制为r = 1.1 + 0.9 − 0.8（在95% C. L.时r <2.8）。如ML流水线所导出的，并且r = 1.2 + 0.9 - 0.8（在95%C.L.下r <2.7）。由PCL管道导出。在其中一个领域，我们发现了与普朗克天空模型的尘埃成分的相关性，尽管与统计误差相比，相应的过剩功率很小。最后，我们推导出所有已知的系统误差的限制，并证明这些对应于一个张量标量比小于r = 0.01，最低水平尚未在文献中报道。
The Q/U Imaging ExperimenT (QUIET) has observed the cosmic microwave background (CMB) at 43 and 95 GHz. The 43 GHz results have been published in a previous paper, and here we report the measurement of CMB polarization power spectra using the 95 GHz data. This data set comprises 5337 hr of observations recorded by an array of 84 polarized coherent receivers with a total array sensitivity of 87 μK. Four low-foreground fields were observed, covering a total of ∼1000 deg2 with an effective angular resolution of 12.′8, allowing for constraints on primordial gravitational waves and high signal-to-noise measurements of the E-modes across three acoustic peaks. The data reduction was performed using two independent analysis pipelines, one based on a pseudo-Cℓ (PCL) cross-correlation approach, and the other on a maximum-likelihood (ML) approach. All data selection criteria and filters were modified until a predefined set of null tests had been satisfied before inspecting any non-null power spectrum. The results derived by the two pipelines are in good agreement. We characterize the EE, EB, and BB power spectra between ℓ = 25 and 975 and find that the EE spectrum is consistent with ΛCDM, while the BB power spectrum is consistent with zero. Based on these measurements, we constrain the tensor-to-scalar ratio to r = 1.1+0.9 − 0.8 (r < 2.8 at 95% C.L.) as derived by the ML pipeline, and r = 1.2+0.9 − 0.8 (r < 2.7 at 95% C.L.) as derived by the PCL pipeline. In one of the fields, we find a correlation with the dust component of the Planck Sky Model, though the corresponding excess power is small compared to statistical errors. Finally, we derive limits on all known systematic errors, and demonstrate that these correspond to a tensor-to-scalar ratio smaller than r = 0.01, the lowest level yet reported in the literature.
影响因子：
8.7
作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者：
Wright, E. L.
DOI：
10.1117/12.787446
发表时间：
2008-07
期刊：
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影响因子：
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作者：
B. Crill;P. Ade;E. Battistelli;S. Benton;R. Bihary;J. Bock;J. Bock;J. Bond;J. Brevik;S. Bryan;C. Contaldi;O. Doré;M. Farhang;L. Fissel;S. Golwala;M. Halpern;G. Hilton;W. Holmes;V. Hristov;K. Irwin;W. Jones;W. Jones;C. Kuo;A. Lange;C. Lawrie;C. MacTavish;T. G. Martin;P. Mason;T. Montroy;C. Netterfield;E. Pascale;D. Riley;J. Ruhl;M. Runyan;A. Trangsrud;C. Tucker;A. Turner;M. Viero;D. Wiebe
通讯作者：
B. Crill;P. Ade;E. Battistelli;S. Benton;R. Bihary;J. Bock;J. Bock;J. Bond;J. Brevik;S. Bryan;C. Contaldi;O. Doré;M. Farhang;L. Fissel;S. Golwala;M. Halpern;G. Hilton;W. Holmes;V. Hristov;K. Irwin;W. Jones;W. Jones;C. Kuo;A. Lange;C. Lawrie;C. MacTavish;T. G. Martin;P. Mason;T. Montroy;C. Netterfield;E. Pascale;D. Riley;J. Ruhl;M. Runyan;A. Trangsrud;C. Tucker;A. Turner;M. Viero;D. Wiebe