标题： 多频率维纳滤波CMB数据与极化 显示英文标题

标题： Multi-frequency Wiener filtering of CMB data with polarisation

摘要： 一个目标是将不同频率、角分辨率和噪声水平的数据结合起来，以最佳地提取具有普朗克谱行为的组分。 在此背景下，Bouchet、Gispert 和 Puget（1995）提出了多频段维纳滤波方法，同时 Tegmark 和 Efstathiou（1996）也独立提出了类似的方法。 如 Bouchet 和 Gispert（1998a）所示，这种线性方法在给定天空模型和实验描述的情况下，也便于先验估计残差误差，假设使用该方法已经去除了前景。 在本文中，我们将该方法扩展到有额外极化数据可用的情况。 特别是，我们推导了涉及极化的功率谱的误差，并给出了未来 CMB 空间任务 MAP 和\plancks \footnote{对于当前的噪声规范以及这些实验的角度和频率覆盖范围，请参见 http://map.gsfc.nasa.gov 和 http://astro.estec.esa.nl/SA-general/Projects/Planck} 的规格数值结果，假设银河系同步辐射和尘埃发射分别约为 40% 和 10% 极化。 我们考虑了两种基础模型用于我们的研究：我们采用一个标准的CDM模型，使用$\tau = 0.1$来提取$E$模式极化和$ET$交叉相关；对于$B$模式极化，我们考虑了一个倾斜的CDM模型，使用$n_s = 0.9, n_T = -0.1$和$T/S = 0.7$。 显示英文摘要

摘要： One goal of CMB data analysis is to combine data at different frequencies, angular resolutions, and noise levels in order to best extract the component with a Plankian spectral behaviour. A multi-frequency Wiener filtering method has been proposed in this context by Bouchet, Gispert and Puget (1995) and in parallel by Tegmark and Efstathiou (1996). As shown in Bouchet and Gispert (1998a), this linear method is also convenient to estimate a priori, given a sky model and an experimental description, the residual errors on the CMB power spectrum assuming the foregrounds have been removed with this method. In this paper, we extend the method to the case when additional polarisation data is available. In particular, we derive the errors on the power spectra involving polarisation and show numerical results for the specifications of the future CMB space missions MAP and \plancks \footnote{For current noise specifications and angular and frequency coverage of these experiments, see http://map.gsfc.nasa.gov and http://astro.estec.esa.nl/SA-general/Projects/Planck} when it is assumed that the Galactic synchrotron and dust emission are respectively about 40% and 10 % polarised. We consider two underlying models for our study: we take a standard CDM model with $\tau = 0.1$ for the extraction of $E$-mode polarisation and $ET$ cross-correlation ; for $B$-mode polarisation we consider a tilted CDM model with $n_s = 0.9, n_T = -0.1$ and $T/S = 0.7$.