BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields-猫眼课题宝

DOI：

10.1103/physrevd.96.102003

发表时间：

2017-05

期刊：

Physical Review D

影响因子：

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

Keck Array;BICEP2 Collaborations P. A. R. Ade;Z. Ahmed;R. Aikin;K. Alexander;D. Barkats;S. Benton;C. Bischoff;J. Bock;R. Bowens-Rubin;J. Brevik;I. Buder;E. Bullock;V. Buza;J. Connors;B. Crill;L. Duband;C. Dvorkin;J. Filippini;S. Fliescher;T. S. Germaine;T. Ghosh;J. Grayson;S. Harrison;S. Hildebrandt;G. Hilton;H. Hui;K. Irwin;J. Kang;K. Karkare;E. Karpel;J. Kaufman;B. Keating;S. Kefeli;S. Kernasovskiy;J. Kovac;C. Kuo;N. Larsen;E. Leitch;K. Megerian;L. Moncelsi;T. Namikawa;C. Netterfield;H. Nguyen;R. O’Brient;IV R.W.Ogburn;C. Pryke;S. Richter;A. Schillaci;R. Schwarz;C. Sheehy;Z. Staniszewski;B. Steinbach;R. Sudiwala;G. Teply;K. Thompson;J. Tolan;C. Tucker;A. Turner;A. Vieregg;A. Weber;D. Wiebe;J. Willmert;C. L. Wong;W. L. K. Wu;K. Yoon

我们提出了迄今为止对宇宙微波背景（CMB）极化旋转各向异性的最强约束，这些极化旋转来自BICEP 2和Keck阵列CMB实验到2014年观测季节（BK 14）的150 GHz数据。BK 14图中偏振角的定义经过了自校准，其中调整整体角度以使观察到的TB和EB功率谱最小化。在此过程之后，QU图失去了对均匀偏振旋转的敏感性，但仍然对偏振旋转的各向异性敏感。这一分析限制了偏振旋转的各向异性，这可能是由CMB光子与类轴赝标场相互作用或由原始磁场诱导的法拉第旋转产生的。BK 14图的灵敏度（1.3 μK−arc min）使其能够重建偏振旋转角的各向异性，并比以前的尝试更精确地测量它们的角功率谱。我们的数据被发现是一致的，没有偏振旋转各向异性，提高旋转角谱的振幅的上限约一个数量级相比，以前的最佳约束。我们的结果导致了对陈-西蒙斯电磁项耦合常数gaγ≤7.2×10−2/HI（95%置信度）的约束比从B模谱导出的约束好一个数量级，其中HI是暴胀哈勃尺度。这一限制导致在质量范围为10−33≤ma≤10−28 eV（r=0.01）时，衰变常数限制为10−6 fa/Mpl，假设gaγ <$α/（2πfa），α表示精细结构常数。从极化旋转各向异性的原始磁场的振幅的上限是30 nG（95%的置信度）。

We present the strongest constraints to date on anisotropies of cosmic microwave background (CMB) polarization rotation derived from 150 GHz data taken by the BICEP2 & Keck Array CMB experiments up to and including the 2014 observing season (BK14). The definition of the polarization angle in BK14 maps has gone through self-calibration in which the overall angle is adjusted to minimize the observed TB and EB power spectra. After this procedure, the QU maps lose sensitivity to a uniform polarization rotation but are still sensitive to anisotropies of polarization rotation. This analysis places constraints on the anisotropies of polarization rotation, which could be generated by CMB photons interacting with axionlike pseudoscalar fields or Faraday rotation induced by primordial magnetic fields. The sensitivity of BK14 maps (∼3μK−arc min) makes it possible to reconstruct anisotropies of the polarization rotation angle and measure their angular power spectrum much more precisely than previous attempts. Our data are found to be consistent with no polarization rotation anisotropies, improving the upper bound on the amplitude of the rotation angle spectrum by roughly an order of magnitude compared to the previous best constraints. Our results lead to an order of magnitude better constraint on the coupling constant of the Chern-Simons electromagnetic term gaγ≤7.2×10−2/HI (95% confidence) than the constraint derived from the B-mode spectrum, where HI is the inflationary Hubble scale. This constraint leads to a limit on the decay constant of 10−6≲fa/Mpl at mass range of 10−33≤ma≤10−28 eV for r=0.01, assuming gaγ∼α/(2πfa) with α denoting the fine structure constant. The upper bound on the amplitude of the primordial magnetic fields is 30 nG (95% confidence) from the polarization rotation anisotropies.

BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields

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