Statistical simulations of the dust foreground to cosmic microwave background polarization (Corrigendum)
Statistical simulations of the dust foreground to cosmic microwave background polarization (Corrigendum)
复制标题
尘埃前景对宇宙微波背景偏振的统计模拟（勘误表）
DOI：
--
复制
发表时间：
2017
影响因子：
6.5
通讯作者：
L. Montier
中科院分区：
文献类型：
--
作者：
F. Vansyngel;F. Boulanger;T. Ghosh;B. Wandelt;J. Aumont;A. Bracco;F. Levrier;P. Martin;L. Montier
宇宙微波背景（CMB）尘埃偏振前景的表征是探测与原始引力波相关的b模信号的必要步骤。我们提出了一种方法来模拟球体上的极化尘埃发射图，类似于对CMB各向异性所做的工作。这种方法建立在对普朗克数据分析所产生的对星系极化的理解之上。它将尘埃极化天空与银河系磁场的结构及其与星际物质和湍流的耦合联系起来。银河系磁场被建模为平均均匀场和随机分量的叠加，幂律功率谱为指数$alpha_{
m m}$。模型参数被约束以拟合利用普朗克数据测量的尘埃极化EE、BB和TE的功率谱。我们发现，当$alpha_{
m m} = -2.5$时，尘埃极化的E和B功率谱斜率是匹配的。该模型允许我们计算Stokes Q和U图的多种实现，以实现磁场的随机成分的不同实现，并量化任何给定的银河面以外的天空区域的尘埃偏振光谱的方差。模拟再现了尘埃极化功率与平均总尘埃强度之间的标度关系，包括在平均关系周围观测到的色散。我们还提出了一种方法来进行多频模拟，包括普朗克最近测量的去相关，使用给定的极化图协方差矩阵。这些模拟非常适合于优化组分分离方法，并在当前和未来的实验中量化尘埃和CMB b模式分离的置信度。我们还为尘埃偏振光谱的建模提供了天体物理学的视角。
The characterization of the dust polarization foreground to the Cosmic Microwave Background (CMB) is a necessary step towards the detection of the B-mode signal associated with primordial gravitational waves. We present a method to simulate maps of polarized dust emission on the sphere, similarly to what is done for the CMB anisotropies. This method builds on the understanding of Galactic polarization stemming from the analysis of Planck data. It relates the dust polarization sky to the structure of the Galactic magnetic field and its coupling with interstellar matter and turbulence. The Galactic magnetic field is modelled as a superposition of a mean uniform field and a random component with a power-law power spectrum of exponent $alpha_{
m M}$. The model parameters are constrained to fit the power spectra of dust polarization EE, BB and TE measured using Planck data. We find that the slopes of the E and B power spectra of dust polarization are matched for $alpha_{
m M} = -2.5$. The model allows us to compute multiple realizations of the Stokes Q and U maps for different realizations of the random component of the magnetic field, and to quantify the variance of dust polarization spectra for any given sky area outside of the Galactic plane. The simulations reproduce the scaling relation between the dust polarization power and the mean total dust intensity including the observed dispersion around the mean relation. We also propose a method to carry out multi-frequency simulations including the decorrelation measured recently by Planck, using a given covariance matrix of the polarization maps. These simulations are well suited to optimize component separation methods and to quantify the confidence with which the dust and CMB B-modes can be separated in present and future experiments. We also provide an astrophysical perspective on our modeling of the dust polarization spectra.
通过同步加速器发射波动研究银河系星际湍流
DOI：
10.1051/0004-6361/201322013
发表时间：
2013
期刊：
Astronomy & Astrophysics
影响因子：
--
作者：
Iacobelli;Haverkorn;Bonafede;Dettmar
通讯作者：
Dettmar
DOI：
10.17863/cam.43425
发表时间：
2016
期刊：
--
影响因子：
--
作者：
Aghanim N
通讯作者：
Aghanim N