BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen-猫眼课题宝

DOI：

10.3847/1538-4357/acb64c

发表时间：

2022-10

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

B. C. P. Ade;Z. Ahmed;M. Amiri;D. Barkats;R. Thakur;D. Beck;C. Bischoff;J. Bock;H. Boenish;E. Bullock;V. Buza;IV J.R.Cheshire;S. Clark;J. Connors;J. Cornelison;M. Crumrine;A. Cukierman;E. Denison;M. Dierickx;L. Duband;M. Eiben;S. Fatigoni;J. Filippini;S. Fliescher;C. Giannakopoulos;N. Goeckner-wald;D. Goldfinger;J. Grayson;P. Grimes;G. Halal;G. Hall;M. Halpern;E. Hand;S. Harrison;S. Henderson;S. Hildebrandt;J. Hubmayr;H. Hui;K. Irwin;J. Kang;K. Karkare;E. Karpel;S. Kefeli;S. A. Kernasovskiy;J. Kovac;C. Kuo;K. Lau;E. Leitch;A. Lennox;K. Megerian;L. Minutolo;L. Moncelsi;Y. Nakato;T. Namikawa;H. T. Nguyen;R. O’Brient;IV R.W.Ogburn;S. Palladino;M. Petroff;T. Prouvé;C. Pryke;B. Racine;C. Reintsema;S. Richter;A. Schillaci;B. Schmitt;R. Schwarz;C. Sheehy;B. Singari;A. Soliman;T. S. Germaine;B. Steinbach;R. Sudiwala;G. Teply;K. Thompson;J. Tolan;C. Tucker;A. Turner;C. Umilta;C. Vergés;A. Vieregg;A. Wandui;A. Weber;D. Wiebe;J. Willmert;C. Wong;W.L.K. Wu;H. Yang;K. Yoon;E. Young;C. Yu;L. Zeng;C. Zhang;S. University;Kipacslac;U. Columbia;HarvardCfA;Caltech;U. Cincinnati;S. University;Nasa Jpl;M. I. O. Astrophysics;U. Chicago;U. Minnesota;Nist;Sbt Grenoble;U. I. Urbana-Champaign;H. University;T. U. O. Tokyo;Aix-Marseille Université;Brookhaven National Laboratory

我们的银河系尘埃丝相关的BICEP/凯克和普朗克数据与偏振模板的基础上中性氢（H i）的观测。尘埃极化对于我们理解星际介质（ISM）中的天体物理过程和在宇宙微波背景（CMB）中寻找原始引力波都是重要的。在弥漫ISM中，H i与尘埃密切相关，并部分组织成与当地磁场对齐的细丝。我们分析了深BICEP/凯克数据在95，150和220 GHz，在低柱密度区域的天空中，BICEP/凯克已经设定了最好的限制原始引力波。我们分离的H i排放到不同的速度分量和检测尘埃偏振与本地银河H i，但不与H i与麦哲伦流i。我们提出了一个强大的，多频检测相关的极化灰尘排放的间接H i形态模板下降到95 GHz。为了评估其前景清洁的效用，我们报告说，高形态模板相关的B模式在一个10%-65%的水平，在多极范围20 <100 <200与BICEP/Keck地图，其中包含来自灰尘，CMB和噪声成分的贡献。测得大气尘埃成分的光谱能量分布的谱指数β = 1.54 ± 0.13。我们没有发现在这个区域的暗条和尘埃场的其余部分之间的去相关的证据，也没有发现与中间速度H i相关的尘埃的存在。最后，我们探讨了基于H i的连续模型中的形态参数空间。

We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H i) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H i is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H i emission into distinct velocity components and detect dust polarization correlated with the local Galactic H i but not with the H i associated with Magellanic Stream i. We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H i morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the Hi morphology template correlates in B modes at a ∼10%–65% level over the multipole range 20 < ℓ < 200 with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be β = 1.54 ± 0.13. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H i. Finally, we explore the morphological parameter space in the H i-based filamentary model.

BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

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