arXiv 1004.35442010-04-28astro-ph.COhep-ph

非均匀宇宙学双折射与活动星系核

Non-Uniform Cosmological Birefringence and Active Galactic Nuclei

Marc Kamionkowski

备注：: 5 pages.
发表信息：: Phys.Rev.D82:047302,2010
DOI：: 10.1103/PhysRevD.82.047302

摘要：

宇宙学双折射是指光子在宇宙学距离上传播时，其偏振方向旋转了一个角度$α$，它受到宇宙微波背景辐射（CMB）的约束，即在整个天空中均匀旋转时，其偏振方向的红移为$|α|\lesssim1^\circ$（$1σ$）。然而，旋转角$α(θ,ϕ)$可以作为天空上的位置$(θ,ϕ)$的函数而变化。在这里，我将讨论如何在当前和未来的活动星系核数据中寻找位置相关的旋转。一个上限$\VEV{α^2}^{1/2} \lesssim 3.7^\circ$的位置-角度-偏振偏移的散射在一个样本中只有N=9活动星系核已经约束的旋转球谐系数$(4π)^{-1/2} α_{lm}\lesssim 3.7^\circ$和约束的功率谱$α$在模型中，它是一个随机场。未来的约束可以改善与更多的来源，并通过分析映射良好的源与张量谐波分解的偏振类似的CMB偏振和弱引力透镜。

英文摘要：

Cosmological birefringence, a rotation by an angle $α$ of the polarization of photons as they propagate over cosmological distances, is constrained by the cosmic microwave background (CMB) to be $|α|\lesssim1^\circ$ ($1σ$) out to redshifts $z\simeq1100$ for a rotation that is uniform across the sky. However, the rotation angle $α(θ,ϕ)$ may vary as a function of position $(θ,ϕ)$ on the sky. Here I discuss how a position-dependent rotation can be sought in current and future AGN data. An upper limit $\VEV{α^2}^{1/2} \lesssim 3.7^\circ$ to the scatter in the position-angle--polarization offsets in a sample of only N=9 AGN already constrains the rotation spherical-harmonic coefficients to $(4π)^{-1/2} α_{lm}\lesssim 3.7^\circ$ and constrains the power spectrum for $α$ in models where it is a stochastic field. Future constraints can be improved with more sources and by analyzing well-mapped sources with a tensor-harmonic decomposition of the polarization analogous to that used in CMB polarization and weak gravitational lensing.

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