The morphology of the thermal Sunyaev-Zel'dovich sky The morphology of the y-sky
The morphology of the thermal Sunyaev-Zel'dovich sky The morphology of the y-sky
复制标题
Sunyaev-Zeldovich 热天空的形态 y 天空的形态
DOI：
10.1111/j.1365-2966.2011.19679.x
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发表时间：
2012
影响因子：
4.8
通讯作者：
Munshi D
中科院分区：
文献类型：
--
作者：
Munshi D
在高的角频率，超出阻尼尾的主要宇宙微波背景（CMB）的功率谱，热Sunyaev-Zel'dovich（tSZ）的影响构成了占主导地位的信号在CMB天空。tSZ效应是由宇宙中重子分布中的大尺度压力波动引起的，因此其统计性质提供了预测的3D压力波动的相应性质的估计。tSZ的功率谱是密度涨落幅度的灵敏探针，双谱可用于分离与压力相关的偏压。双谱通常用它的一点实空间模拟，偏度来探测。除了普通的偏度的形态属性，由著名的闵可夫斯基泛函探测，还需要广义一点统计，这在最低阶是相同的广义偏度参数。广义偏态参数的概念可以进一步扩展到定义一组三个相关联的广义偏态谱。我们使用这些倾斜光谱来探测tSZ天空或y天空的形态。我们展示了如何可以恢复这些功率谱的数据中存在的任意的掩模和噪声模板，使用众所周知的伪Clapproach任意波束形状。我们还采用了基于晕模型的方法来计算tSZ双谱。然后使用这些模型的双谱来构造广义斜谱。我们考虑的性能与普朗克型噪声的全天空调查和比较的结果与无噪声的理想实验，使用一系列的平滑角。我们发现，偏态谱可以估计非常高的信噪比从未来的频率清洁tSZ地图，将可从实验asPlanck。这将允许他们的模式，模式的估计，为广泛的角频率和将帮助我们区分他们从其他来源的非高斯。
At high angular frequencies, beyond the damping tail of the primary cosmic microwave background (CMB) power spectrum, the thermal Sunyaev–Zel’dovich (tSZ) effect constitutes the dominant signal in the CMB sky. The tSZ effect is caused by large-scale pressure fluctuations in the baryonic distribution in the universe, such that its statistical properties provide estimates of corresponding properties of the projected 3D pressure fluctuations. The power spectrum of the tSZ is a sensitive probe of the amplitude of density fluctuations, and the bispectrum can be used to separate the bias associated with the pressure. The bispectrum is typically probed with its one-point real-space analogue, the skewness. In addition to the ordinary skewness the morphological properties, as probed by the well-known Minkowski functionals, also require the generalized one-point statistics, which at the lowest order are identical to the generalized skewness parameters. The concept of generalized skewness parameters can be further extended to define a set of three associated generalizedskew-spectra. We use these skew-spectra to probe the morphology of the tSZ sky or the y-sky. We show how these power spectra can be recovered from the data in the presence of an arbitrary mask and noise templates using the well known pseudo-Clapproach for arbitrary beam shape. We also employ an approach based on the halo model to compute the tSZ bispectrum. The bispectrum from each of these models is then used to construct the generalized skew-spectra. We consider the performance of an all-sky survey withPlanck-type noise and compare the results against a noise-free ideal experiment using a range of smoothing angles. We find that the skew-spectra can be estimated with very high signal-to-noise ratio from future frequency-cleaned tSZ maps that will be available from experiments such asPlanck. This will allow theirmode-by-modeestimation for a wide range of angular frequenciesland will help us distinguish them from other sources of non-Gaussianity.