Full-sky, Arcminute-scale, 3D Models of Galactic Microwave Foreground Dust Emission Based on Filaments
Full-sky, Arcminute-scale, 3D Models of Galactic Microwave Foreground Dust Emission Based on Filaments
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DOI：
10.3847/1538-4357/ac54b2
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发表时间：
2021-07
期刊：
影响因子：
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通讯作者：
C. Herv'ias-Caimapo;K. Huffenberger
中科院分区：
文献类型：
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作者：
C. Herv'ias-Caimapo;K. Huffenberger
我们给出了尘埃细丝代码，这是一种银河系毫米级热尘埃排放的全天模型。我们的模型由数百万条与磁场不完全对齐的细丝组成，能够再现普朗克任务测量的353 GHz尘埃角功率谱的主要特征。我们的模型由一组细丝组成，其大小服从帕累托分布∝La−2.445，短半轴和长半轴的轴比ϵ∼为0.16，磁场失准角的色散均方根(θLh)=10°。在大尺度上，我们的模型遵循基于普朗克的模板。在小尺度上，我们的模型通过考虑更小的灯丝产生的光谱行为类似于ℓ∼4000或更小的尺度的幂定律，仅受计算能力的限制。我们可以产生任意数量的小尺度银河系尘埃的蒙特卡罗实现。我们的模型将允许测试小规模非高斯性如何影响CMB弱透镜，以及对原始引力波或相对论光遗迹物种的测量结果。我们的模型还可以在修正后的尘埃黑体光谱上产生频率去相关，并且可以自由调整到不同程度的去相关。这可以用来测试分量分离方法的性能以及频谱残差对原始B型测量的影响。我们在天空中绘制的灯丝密度也能够重现普朗克353 GHz频道图中Minkowski泛函测量的非高斯泛函的一般水平。
We present the DustFilaments code, a full-sky model for the millimeter Galactic emission of thermal dust. Our model, composed of millions of filaments that are imperfectly aligned with the magnetic field, is able to reproduce the main features of the dust angular power spectra at 353 GHz as measured by the Planck mission. Our model is made up of a population of filaments with sizes following a Pareto distribution ∝La−2.445 , with an axis ratio between short and long semiaxes ϵ ∼ 0.16 and an angle of magnetic field misalignment with a dispersion rms(θ LH) = 10°. On large scales, our model follows a Planck-based template. On small scales, our model produces spectra that behave like power laws up to ℓ ∼ 4000 or smaller scales by considering even smaller filaments, limited only by computing power. We can produce any number of Monte Carlo realizations of small-scale Galactic dust. Our model will allow tests of how the small-scale non-Gaussianity affects CMB weak lensing and the consequences for the measurement of primordial gravitational waves or relativistic light relic species. Our model also can generate frequency decorrelation on the modified blackbody spectrum of dust and is freely adjustable to different levels of decorrelation. This can be used to test the performance of component separation methods and the impact of frequency spectrum residuals on primordial B-mode surveys. The filament density we paint in the sky is also able to reproduce the general level of non-Gaussianities measured by Minkowski functionals in the Planck 353 GHz channel map.