The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ

DOI：

10.1088/1475-7516/2014/10/007

发表时间：

2014-05

期刊：

Journal of Cosmology and Astroparticle Physics

影响因子：

6.4

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

S. Naess;M. Hasselfield;J. McMahon;M. Niemack;G. Addison;P. Ade;R. Allison;M. Amiri;N. Battaglia;J. Beall;F. Bernardis;J. Bond;J. Britton;E. Calabrese;Hsiao-mei Cho.;K. Coughlin;D. Crichton;Sudeep Das;R. Datta;M. Devlin;S. Dicker;J. Dunkley;R. Dunner;J. Fowler;A. Fox;P. Gallardo;E. Grace;M. Gralla;A. Hajian;M. Halpern;S. Henderson;J. Hill;G. Hilton;M. Hilton;A. Hincks;R. Hložek;P. Ho;J. Hubmayr;K. Huffenberger;J. Hughes;L. Infante;K. Irwin;Rebecca Jackson;S. M. Kasanda;J. Klein;B. Koopman;A. Kosowsky;Dale Li;T. Louis;M. Lungu;M. Madhavacheril;T. Marriage;L. Maurin;F. Menanteau;K. Moodley;C. Munson;L. Newburgh;J. Nibarger;M. Nolta;L. Page;C. Pappas;B. Partridge;F. Rojas;B. Schmitt;N. Sehgal;B. Sherwin;J. Sievers;S. Simon;D. Spergel;S. Staggs;E. Switzer;R. Thornton;H. Trac;C. Tucker;M. Uehara;A. V. Engelen;J. Ward;Edward J. Wollack

我们报告了阿塔卡马宇宙望远镜偏振计（ACTPol）在其观测的前三个月对宇宙微波背景（CMB）和146 GHz天体偏振的测量结果。天空的四个区域共覆盖270平方度，以1.3 '的角分辨率绘制。4个区域的地图噪声水平在11 ~ 17 μK-arcmin之间。我们给出了其中三个区域的TT、TE、EE、TB、EB和BB功率谱。观测到的e模极化功率谱在200 < l < 3000范围内有6个声峰，与WMAP9+ACT和普朗克数据预测的最佳拟合宇宙学模型非常吻合。偏振功率谱主要反映原始等离子体速度扰动，它提供了一个独立的宇宙学参数确定，与基于温度功率谱的宇宙学参数确定一致，温度功率谱主要来自原始密度扰动。我们发现，在不掩盖任何点源的情况下，在95%置信度下，由于极化点源引起的EE功率谱泊松尾在r = 3000处的振幅小于2.4 μ 2。最后，我们报道了蟹状星云作为一个重要的微波偏振定标源，经过5′高斯波束平滑后，其偏振角为150.7±0.6°，为8.7%。

We report on measurements of the cosmic microwave background (CMB) and celestial polarization at 146 GHz made with the Atacama Cosmology Telescope Polarimeter (ACTPol) in its first three months of observing. Four regions of sky covering a total of 270 square degrees were mapped with an angular resolution of 1.3′. The map noise levels in the four regions are between 11 and 17 μK-arcmin. We present TT, TE, EE, TB, EB, and BB power spectra from three of these regions. The observed E-mode polarization power spectrum, displaying six acoustic peaks in the range 200 < ℓ < 3000, is an excellent fit to the prediction of the best-fit cosmological models from WMAP9+ACT and Planck data. The polarization power spectrum, which mainly reflects primordial plasma velocity perturbations, provides an independent determination of cosmological parameters consistent with those based on the temperature power spectrum, which results mostly from primordial density perturbations. We find that without masking any point sources in the EE data at ℓ < 9000, the Poisson tail of the EE power spectrum due to polarized point sources has an amplitude less than 2.4 μ 2 at ℓ = 3000 at 95% confidence. Finally, we report that the Crab Nebula, an important polarization calibration source at microwave frequencies, has 8.7% polarization with an angle of 150.7̂ ± 0.6̂ when smoothed with a 5′ Gaussian beam.

The Atacama Cosmology Telescope: CMB polarization at 200 < ℓ < 9000

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